explanation      blue bibcodes open ADS page with paths to full text
Author name code: haisch
ADS astronomy entries on 2022-09-14
author:"Haisch, Bernard M." 

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Title: The Cosmos Portal and the IYA2009 Project
Authors: Haisch, Bernard M.; Sims, M.; Lindblom, J.
2009AAS...21440001H    Altcode:
  In 2007 the non-profit Digital Universe Foundation (DUF) launched the
  Earth Portal (earthportal.org) as a comprehensive resource for timely,
  objective, science-based information about the environment. There are
  currently over 1000 scholars from 60 countries engaged in this rapidly
  growing web-based collaboration. The Cosmos Portal is the second major
  DUF initiative (cosmosportal.org). In support of the IYA2009 effort, the
  Cosmos Portal is recruiting astronomy professionals to make use of easy
  online tools to publish articles, blogs, news items, image galleries,
  class notes, lectures, powerpoint presentations, links to other high
  quality websites or other educational material. A major difference
  between the Digital Universe and Wikipedia is that educational material
  is produced by identified experts, not anonymous contributors with
  unknown qualifications. The Digital Universe is a 501(c)(3) public
  charity whose goal is to evolve into a worldwide online community
  (a social network) whose centerpiece is an ever growing Asimov-Sagan
  Encyclopedia Galactica created by experts. We encourage you to write
  an encylopedia article or start a portal on your favorite topic or
  join an existing topic as an expert contributor.

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Title: The Cosmos Portal and the IYA2009 Project
Authors: Haisch, Bernard M.; Sims, M.; Lindblom, J.
2009AAS...21346508H    Altcode: 2009BAAS...41..413H
  In 2007 the non-profit Digital Universe Foundation (DUF) launched
  the Earth Portal as a comprehensive resource for timely, objective,
  science-based information about the environment. There are currently
  over 1000 scholars from 60 countries engaged in this rapidly growing
  web-based collaboration. The Cosmos Portal is the second major DUF
  initiative (digitaluniverse.net/cosmos). In support of the IYA2009
  effort, the Cosmos Portal is recruiting astronomy professionals to
  make use of easy online tools to publish articles, blogs, news items,
  image galleries, class notes, lectures, powerpoint presentations,
  links to other high quality websites or other educational material. In
  parallel we intend to bring hundreds of amateur astronomy organizations
  and thousands of amateur astronomers and telescope makers together in
  a community of portals (digitaluniverse.net/cosmoscommunity). This
  will allow vibrant online collaboration and information sharing. We
  encourage you to start a portal on your favorite topic or join an
  existing topic as a contributor.

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Title: Astronomy in the Digital Universe
Authors: Haisch, Bernard M.; Lindblom, J.; Terzian, Y.
2006AAS...209.9402H    Altcode: 2006BAAS...38.1031H
  The Digital Universe is an Internet project whose mission is to provide
  free, accurate, unbiased information covering all aspects of human
  knowledge, and to inspire humans to learn, make use of, and expand this
  knowledge. It is planned to be a decades long effort, inspired by the
  Encyclopedia Galactica concept popularized by Carl Sagan, and is being
  developed by the non-profit Digital Universe Foundation. A worldwide
  network of experts is responsible for selecting content featured
  within the Digital Universe. The first publicly available content
  is the Encyclopedia of Earth, a Boston University project headed by
  Prof. Cutler Cleveland, which will be part of the Earth Portal. The
  second major content area will be an analogous Encyclopedia of the
  Cosmos to be part of the Cosmos Portal. It is anticipated that this will
  evolve into a major resource for astronomy education. Authors and topic
  editors are now being recruited for the Encyclopedia of the Cosmos.

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Title: Review of Experimental Concepts for Studying the Quantum
    Vacuum Field
Authors: Davis, E. W.; Teofilo, V. L.; Haisch, B.; Puthoff, H. E.;
   Nickisch, L. J.; Rueda, A.; Cole, D. C.
2006AIPC..813.1390D    Altcode:
  We review concepts that provide an experimental framework for exploring
  the possibility and limitations of accessing energy from the space
  vacuum environment. Quantum electrodynamics (QED) and stochastic
  electrodynamics (SED) are the theoretical approaches guiding this
  experimental investigation. This investigation explores the question
  of whether the quantum vacuum field contains useful energy that can be
  exploited for applications under the action of a catalyst, or cavity
  structure, so that energy conservation is not violated. This is similar
  to the same technical problem at about the same level of technology
  as that faced by early nuclear energy pioneers who searched for, and
  successfully discovered, the unique material structure that caused
  the release of nuclear energy via the neutron chain reaction.

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Title: Gravity and the quantum vacuum inertia hypothesis
Authors: Rueda, A.; Haisch, B.
2005AnP...517..479R    Altcode: 2005gr.qc.....4061R; 2005AnP....14..479R
  In previous work it has been shown that the electromagnetic quantum
  vacuum, or electromagnetic zero-point field, makes a contribution to
  the inertial reaction force on an accelerated object. We show that
  the result for inertial mass can be extended to passive gravitational
  mass. As a consequence the weak equivalence principle, which equates
  inertial to passive gravitational mass, appears to be explainable. This
  in turn leads to a straightforward derivation of the classical Newtonian
  gravitational force. We call the inertia and gravitation connection
  with the vacuum fields the quantum vacuum inertia hypothesis. To date
  only the electromagnetic field has been considered. It remains to
  extend the hypothesis to the effects of the vacuum fields of the other
  interactions. We propose an idealized experiment involving a cavity
  resonator which, in principle, would test the hypothesis for the simple
  case in which only electromagnetic interactions are involved. This
  test also suggests a basis for the free parameter $\eta(\nu)$ which we
  have previously defined to parametrize the interaction between charge
  and the electromagnetic zero-point field contributing to the inertial
  mass of a particle or object.

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Title: The Virtual Cosmos Project: Astronomical Data access for
    General Public via the National Virtual Observatory
Authors: Craig, N.; Mendez, B. J.; Hanisch, R. J.; Christian, C. A.;
   Summers, F.; Haisch, B.; Lindblom, J.
2005AAS...206.0509C    Altcode: 2005BAAS...37..435C
  We will describe the development of protocols to make Astronomy
  press-release quality images from HST and other sources publicly
  available through compatibility with the National Virtual Observatory
  (NVO). We will present the designs for a public portal to these
  resources, based on a robust evaluation of our intended audience. The
  availability of press-release quality materials via the NVO through
  a simplified interface will greatly enhance the utility of these
  materials for the public. Behind any portal to NVO data there is a
  standard registry and data structures that allow collections of data
  (such as the press release images) to be located and acquired. We will
  describe our design of the necessary protocols and metadata being used
  within the NVO framework for this project. We base our meta-tags on
  the considerable existing work done in the science community as well
  as the NASA education community. These refined metadata are applied
  to new HST press-release images as they are produced and registered
  with the NVO. We will describe methods for retrofitting pre-existing
  imagery with the metadata standards. The rich media, 3D navigation and
  visualization capabilities of the browser created by ManyOne Network
  Inc. are particularly well suited to the presentation of astronomical
  information and ever more detailed models of the local neighborhood,
  the Milky Way, etc. We will discuss the 3D navigation and visualization
  capabilities of the browser with particular focus on the Milky Way
  Galaxy. Development of an online encyclopedia to accompany the ManyOne
  portals as part of the Virtual Cosmos will also be described. Support
  from NASA's AISR Program is gratefully acknowledged.

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Title: Inflation-Theory Implications for Extraterrestrial Visitation
Authors: Deardoff, J.; Haisch, B.; Maccabee, B.; Puthoff, H. E.
2005JBIS...58...43D    Altcode:
  It has recently been argued that anthropic reasoning applied to
  inflation theory reinforces the prediction that we should find ourselves
  part of a large, galaxy-sized civilisation, thus strengthening Fermi's
  paradox concerning `Where are they?' Furthermore, superstring and
  M-brane theory allow for the possibility of parallel universes, some of
  which in principle could be habitable. In addition, discussion of such
  exotic transport concepts as `traversable wormholes' now appears in the
  rigorous physics literature. As a result, the `We are alone' solution
  to Fermi's paradox, based on the constraints of earlier 20th century
  viewpoints, appears today to be inconsistent with new developments
  in our best current physics and astrophysics theories. Therefore we
  reexamine and reevaluate the present assumption that extraterrestrials
  or their probes are not in the vicinity of Earth, and argue instead that
  some evidence of their presence might be found in certain high-quality
  UFO reports. This study follows up on previous arguments that (1)
  interstellar travel for advanced civilizations is not a priori ruled
  out by physical principles and therefore may be practicable, and (2)
  such advanced civilisations may value the search for knowledge from
  uncontaminated species more than direct, interspecies communication,
  thereby accounting for apparent covertness regarding their presence.

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Title: The Digital Universe Coalition: Building a Prototype NVO
    E/PO Portal
Authors: Mendez, B.; Craig, N.; Haisch, B.; Lindblom, J.; Hanisch,
   R.; Summers, F.; Abbott, B.
2004AAS...204.7805M    Altcode: 2004BAAS...36..810M
  The National Virtual Observatory (NVO) holds tremendous potential for
  Education and Public Outreach (E/PO) opportunities. The possibilities
  for E/PO with the NVO, which promises to make widely available the
  great majority of the world's astronomical data, are too numerous for
  any one E/PO effort to ever hope to develop. Therefore, it is critical
  that the NVO E/PO program develop an infrastructure and tools flexible
  enough that any E/PO program can make use of it. In response to the
  recommendations of the NVO science definition team, UC Berkeley's SEGway
  program conducted needs assessment surveys of potential non-traditional
  (i.e. non-scientist) NVO user communities. The SEGway team wished to
  use the results of these surveys to design a demonstration website
  that could show some of the potential capabilities of NVO E/PO. SEGway
  established an informal partnership with STScI, AMNH/Hayden Planetarium,
  and ManyOne Network to explore how to assemble the infrastructure
  and tools for NVO E/PO and to construct a demonstration portal that
  makes use of NVO resources. We called this partnership The Digital
  Universe Coalition. This prototype displays AMNH/Hayden's Digital
  Universe star catalog of approximately 100,000 stars, based largely
  on HIPPARCOS parallaxes, in a virtual three-dimensional space. Three
  types of user-interactive data display and/or navigation are possible:
  an Earth-based view of the sky with the option of displaying
  constellations; a spaceship-based view moving through space; and a
  "god's-eye" view of the local neighborhood from an external vantage
  point. One key feature of this demo is the linking of user-selectable
  locations in the sky to the online Digitized Sky Survey data sets. A
  second feature is a set of links for educational content on a handful of
  selected objects. Both of these capabilities will be extended further
  as we plan to begin development of a much more robust and complete
  E/PO portal for the NVO.

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Title: Update on an Electromagnetic Basis for Inertia, Gravitation,
    the Principle of Equivalence, Spin and Particle Mass Ratios
Authors: Haisch, Bernard; Rueda, Alfonso; Nickisch, L. J.; Mollere,
   Jules
2003AIPC..654..922H    Altcode: 2002gr.qc.....9016H
  A possible connection between the electromagnetic quantum vacuum and
  inertia was first published by Haisch, Rueda and Puthoff (1994). If
  correct, this would imply that mass may be an electromagnetic
  phenomenon and thus in principle subject to modification, with possible
  technological implications for propulsion. A multiyear NASA-funded study
  at the Lockheed Martin Advanced Technology Center further developed
  this concept, resulting in an independent theoretical validation of
  the fundamental approach (Rueda and Haisch, 1998ab). Distortion of the
  quantum vacuum in accelerated reference frames results in a force that
  appears to account for inertia. We have now shown that the same effect
  occurs in a region of curved spacetime, thus elucidating the origin
  of the principle of equivalence (Rueda, Haisch and Tung, 2001). A
  further connection with general relativity has been drawn by Nickisch
  and Mollere (2002): zero-point fluctuations give rise to spacetime
  micro-curvature effects yielding a complementary perspective on the
  origin of inertia. Numerical simulations of this effect demonstrate
  the manner in which a massless fundamental particle, e.g. an electron,
  acquires inertial properties; this also shows the apparent origin of
  particle spin along lines originally proposed by Schroedinger. Finally,
  we suggest that the heavier leptons (muon and tau) may be explainable
  as spatial-harmonic resonances of the (fundamental) electron. They
  would carry the same overall charge, but with the charge now having
  spatially lobed structure, each lobe of which would respond to higher
  frequency components of the electromagnetic quantum vacuum, thereby
  increasing the inertia and thus manifesting a heavier mass.

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Title: The Inertia Reaction Force and Its Vacuum Origin
Authors: Rueda, Alfonso; Haisch, Bernard
2003grco.book..447R    Altcode:
  By means of a covariant approach we show that there must be a
  contribution to the inertial mass and to the inertial reaction force
  on an accelerated massive object by the zero-point electromagnetic
  field. This development does not require any detailed model of
  the accelerated object other than the knowledge that it interacts
  electromagnetically. It is shown that inertia can indeed be construed
  as an opposition of the vacuum fields to any change to the uniform
  state of motion of an object. Interesting insights originating from
  this result are discussed. It is argued why the proposed existence
  of a Higgs field in no way contradicts or is at odds with the above
  statements. The Higgs field is responsible for assigning mass to
  elementary particles. It is argued that still the underlying reason for
  the opposition to acceleration that massive objects present requires
  an explanation. The explanation proposed here fulfills that requirement.

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Title: A Lot of Observations of the Coronae of AR Lac
Authors: Pease, D.; Drake, J. J.; Kashyap, V.; Ratzlaff, P. W.; Saar,
   S.; Haisch, B.; Dobrzycki, A.; Adams, N. R.; Wolk, S. J.
2002ASPC..277..551P    Altcode: 2002sccx.conf..551P
  No abstract at ADS

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Title: The Inertia Reaction Force and its Vacuum Origin
Authors: Rueda, Alfonso; Haisch, Bernard
2002gchr.conf..447R    Altcode:
  No abstract at ADS

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Title: Gravity and the Quantum Vacuum Inertia
    Hypothesis. I. Formalized Groundwork for Extension to Gravity
Authors: Rueda, Alfonso; Haisch, Bernard; Tung, Roh
2001gr.qc.....8026R    Altcode:
  It has been shown [1,2] that the electromagnetic quantum vacuum makes
  a contribution to the inertial mass, $m_i$, in the sense that at least
  part of the inertial force of opposition to acceleration, or inertia
  reaction force, springs from the electromagnetic quantum vacuum. As
  experienced in a Rindler constant acceleration frame the electromagnetic
  quantum vacuum mainfests an energy-momentum flux which we call the
  Rindler flux (RF). The RF, and its relative, Unruh-Davies radiation,
  both stem from event-horizon effects in accelerating reference
  frames. The force of radiation pressure produced by the RF proves to be
  proportional to the acceleration of the reference frame, which leads to
  the hypothesis that at least part of the inertia of an object should
  be due to the interaction of its quarks and electrons with the RF. We
  demonstrate that this quantum vacuum inertia hypothesis is consistent
  with general relativity (GR) and that it answers a fundamental question
  left open within GR, viz. is there a physical mechanism that generates
  the reaction force known as weight when a specific non-geodesic motion
  is imposed on an object? The quantum vacuum inertia hypothesis provides
  such a mechanism, since by assuming the Einstein principle of local
  Lorentz-invariance (LLI), we can immediately show that the same RF
  arises due to curved spacetime geometry as for acceleration in flat
  spactime. Thus the previously derived expression for the inertial mass
  contribution from the electromagnetic quantum vacuum field is exactly
  equal to the corresponding contribution to the gravitational mass,
  $m_g$. Therefore, within the electromagnetic quantum vacuum viewpoint
  proposed in [1,2], the Newtonian weak equivalence principle, $m_i=m_g$,
  ensues in a straightforward manner.

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Title: Geometrodynamics, Inertia and the Quantum Vacuum
Authors: Haisch, Bernard; Rueda, Alfonso
2001gr.qc.....6075H    Altcode:
  Why does {\bf F} equal m{\bf a} in Newton's equation of motion? How
  does a gravitational field produce a force? Why are inertial mass
  and gravitational mass the same? It appears that all three of
  these seemingly axiomatic foundational questions have an answer
  involving an identical physical process: interaction between the
  electromagnetic quantum vacuum and the fundamental charged particles
  (quarks and electrons) constituting matter. All three of these effects
  and equalities can be traced back to the appearance of a specific
  asymmetry in the otherwise uniform and isotropic electromagnetic
  quantum vacuum. This asymmetry gives rise to a non-zero Poynting vector
  from the perspective of an accelerating object. We call the resulting
  energy-momentum flux the {\it Rindler flux}. The key insight is that
  the asymmetry in an accelerating reference frame in flat spacetime
  is identical to that in a stationary reference frame (one that is
  not falling) in curved spacetime. Therefore the same Rindler flux
  that creates inertial reaction forces also creates weight. All of
  this is consistent with the conceptualizaton and formalism of general
  relativity. What this view adds to physics is insight into a specific
  physical process creating identical inertial and gravitational forces
  from which springs the weak principle of equivalence. What this view
  hints at in terms of advanced propulsion technology is the possibility
  that by locally modifying either the electromagnetic quantum vacuum
  and/or its interaction with matter, inertial and gravitational forces
  could be modified.

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Title: Inertial mass and the quantum vacuum fields
Authors: Haisch, Bernard; Rueda, Alfonso; Dobyns, York
2001AnP...513..393H    Altcode: 2001AnP....10..393H; 2000gr.qc.....9036H
  Even when the Higgs particle is finally detected, it will continue
  to be a legitimate question to ask whether the inertia of matter as
  a reaction force opposing acceleration is an intrinsic or extrinsic
  property of matter. General relativity specifies which geodesic path a
  free particle will follow, but geometrodynamics has no mechanism for
  generating a reaction force for deviation from geodesic motion. We
  discuss a different approach involving the electromagnetic zero-point
  field (ZPF) of the quantum vacuum. It has been found that certain
  asymmetries arise in the ZPF as perceived from an accelerating reference
  frame. In such a frame the Poynting vector and momentum flux of the ZPF
  become non-zero. Scattering of this quantum radiation by the quarks and
  electrons in matter can result in an acceleration-dependent reaction
  force. Both the ordinary and the relativistic forms of Newton's second
  law, the equation of motion, can be derived from the electrodynamics
  of such ZPF-particle interactions. Conjectural arguments are given
  why this interaction should take place in a resonance at the Compton
  frequency, and how this could simultaneously provide a physical basis
  for the de Broglie wavelength of a moving particle. This affords a
  suggestive perspective on a deep connection between electrodynamics,
  the origin of inertia and the quantum wave nature of matter.

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Title: How to Abhor the Void While Loving the Quantum Vacuum
Authors: Haisch, Bernard; Rueda, Alfonso
2000Mercu..29e..32H    Altcode:
  Getting to another star in a human lifetime right now seems impossible,
  but intriguing physics offers us some fantastic possibilities to
  consider.

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Title: Prospects for an Interstellar Mission: Hard Technology Limits
    but Surprising Physics Possibilities
Authors: Haisch, Bernard; Rueda, Alfonso
2000Mercu..29d..26H    Altcode:
  How can we reach another star in a timely fashion? Extrapolating our
  best current technology into the future is like trying to somehow
  soup-up Magellan's sailing ship to circumnavigate the globe in ninety
  minutes.

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Title: On the relation between a zero-point-field-induced inertial
    effect and the Einstein-de Broglie formula
Authors: Haisch, Bernard; Rueda, Alfonso
2000PhLA..268..224H    Altcode: 1999gr.qc.....6084H
  It has been proposed that the scattering of electromagnetic zero-point
  radiation by accelerating objects results in a reaction force
  that may account, at least in part, for inertia [1-3]. This arises
  because of asymmetries in the electromagnetic zero-point field (ZPF)
  or electromagnetic quantum vacuum as perceived from an accelerating
  reference frame. In such a frame, the Poynting vector and momentum
  flux of the ZPF become non-zero. If one assumes that scattering of
  the ZPF radiation takes place at the level of quarks and electrons
  constituting matter, then it is possible for both Newton's equation of
  motion, f=ma, and its relativistic covariant generalization, F=dP/dτ,
  to be obtained as a consequence of the non-zero ZPF momentum flux. We
  now conjecture that this scattering must take place at the Compton
  frequency of a particle, and that this interpretation of mass leads
  directly to the de Broglie relation characterizing the wave nature of
  that particle in motion, λ<SUB>B</SUB>=h/p. This suggests a perspective
  on a connection between electrodynamics and the quantum wave nature
  of matter. Attempts to extend this perspective to other aspects of
  the vacuum are left for future consideration.

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Title: The Case for Inertia as a Vacuum Effect: A Reply to Woodward
    and Mahood
Authors: Dobyns, York; Rueda, Alfonso; Haisch, Bernard
2000gr.qc.....2069D    Altcode:
  The possibility of an extrinsic origin for inertial reaction forces has
  recently seen increased attention in the physical literature. Among
  theories of extrinsic inertia, the two considered by the current
  work are (1) the hypothesis that inertia is a result of gravitational
  interactions, and (2) the hypothesis that inertial reaction forces arise
  from the interaction of material particles with local fluctuations
  of the quantum vacuum. A recent article supporting the former and
  criticizing the latter is shown to contain substantial errors.

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Title: Physical Requirements for Flares in Stars
Authors: Haisch, B.
2000ASPC..214..304H    Altcode: 2000bpet.conf..304H; 2000IAUCo.175..304H
  No abstract at ADS

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Title: Solar-Stellar Connection
Authors: Haisch, B. M.
1999mfs..conf..481H    Altcode:
  Stellar Coronae and Acoustic Heating The Dividing Line the
  Rotation-Activity Relation: Calibrating the Dynamo Age Versus Activity:
  The Evolution of the Sun Stellar Activity Cycles Mapping Stellar
  Surfaces Flares on Other Stars What is the Range of Stellar Power
  Ratios? Conclusion

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Title: Active Regions
Authors: Holman, G. D.; Cheng, C. -C.; Gurman, J. B.; Haisch, B. M.;
   Poland, A. I.; Porter, J. G.; Saba, J. L. R.; Schmieder, B.; Strong,
   K. T.
1999mfs..conf...41H    Altcode:
  Magnetic Field Strength and Strucutre Results Prior to SMM First Results
  with SMM Subsequent Results: 1983-1987 The Coronal Magnetic Structures
  Observing Campaign Coronal Magnetic Field Studies after SMM Dynamics
  and Heating of the Solar Corona FCS Line-Broadening Measurements
  Large Nonthermal Velocities Spatial Variations Correlation Studies FCS
  Line-Broadening Data Interpreting the FCS Line Broadening Constraints
  on Mass Motions Link to Heating Discussion Coronal Heating, Magnetic
  Fields, and Flares UVSP Obervations of Active Regions Transition Region
  Brightenings: UV Microflares Sunspots Magnetic Field and Height of the
  Transition Region Sunspot Plumes Sunspot Flows Horizontal Flows Vertical
  Flows Nonthermal Line Broadening Umbral Oscillations A Look Backward,
  a Look Forward Prominences and Filaments Prominence Environment and
  Structure Steady Flows in Prominence Material Activity in Prominences
  Postflare Loops and Surges Conclusion

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Title: A Geosynchronous 2.4-meter UV/Optical Astrophysical Observatory
Authors: Haisch, B.; Robb, P.; Strong, K.; Shemansky, D.
1999ASPC..164..279H    Altcode: 1999uosa.conf..279H
  No abstract at ADS

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Title: Design for a low-cost, 2.4-meter, geosynchronous UV Observatory
Authors: Haisch, B.; Robb, P.; Strong, K.; Shemansky, D.
1998AAS...192.8003H    Altcode: 1998BAAS...30..935H
  Studies were initiated in 1995 at the Lockheed Martin Advanced
  Technology Center in Palo Alto to explore both the application of new
  technologies and the economical utilization of commercial products to
  the design of a new generation of scientific research satellites. A
  2.4-meter Solar System Observatory (SSO) has been designed to carry
  out as its primary mission imaging and spectroscopy of comets and
  of the outer planets from geosynchronous orbit. Such a Hubble-class
  telescope with a science payload consisting of four UV/EUV spectrographs
  (wavelength range 550-3200 Angstroms , spectral resolution up to 20000)
  and a high-resolution imager having 0.06 arcsec spatial resolution
  can now be built and launched within the budget of a NASA Discovery
  Mission. Following a one-year science program under the direction of the
  principal investigator, the SSO would transition to a guest observer
  facility. Although optimized for cometary and planetary measurements
  in the UV/EUV, SSO would have outstanding capability for a variety
  of astrophysical measurements in the UV. SSO would also serve as a
  prototype for other similar low-cost space observatories that could
  be optimized for stellar, extragalactic and other applications.

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Title: A Telescope Design for Direct Imaging of Extrasolar Planets
Authors: Robb, P.; Bandermann, L.; Haisch, B.; Strong, K.
1998AAS...192.8004R    Altcode: 1998BAAS...30..935R
  We report on the design of a 2.0-meter orbiting telescope capable of
  detection by direct imaging of Jupiter-class planets around solar-type
  stars at a distance of up to 10 parsecs. The telescope would operate
  in the visible spectrum, using reflected light to maximize angular
  resolution. An off-axis Gregorian telescope with field and Lyot
  stops has been designed using low-scatter mirror surfaces and optical
  apodization to control diffraction. Calculations indicate that the
  system will reliably detect Jupiter- and Saturn-class planets around
  solar-type stars at angular separations as small as 0.5 arcsec. Such
  a single-telescope system would fit within the constraints of a
  Discovery or MIDEX NASA program, and would serve as a pathfinder for
  large space-based interferometric systems.

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Title: The Zero-Point Field and Inertia
Authors: Haisch, B.; Rueda, A.
1998clmp.conf..171H    Altcode: 1999gr.qc.....8057H
  A brief overview is presented of the basis of the electromagnetic
  zero-point field in quantum physics and its representation in stochastic
  electrodynamics. Two approaches have led to the proposal that the
  inertia of matter may be explained as an electromagnetic reaction
  force. The first is based on the modeling of quarks and electrons
  as Planck oscillators and the method of Einstein and Hopf to treat
  the interaction of the zero-point field with such oscillators. The
  second approach is based on analysis of the Poynting vector of the
  zero-point field in accelerated reference frames. It is possible to
  derive both Newton's equation of motion, F=ma, and its relativistic
  co-variant form from Maxwell's equations as applied to the zero-point
  field of the quantum vacuum. This appears to account, at least in part,
  for the inertia of matter.

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Title: Electromagnetic Vacuum and Inertial Mass
Authors: Rueda, A.; Haisch, B.
1998clmp.conf..179R    Altcode:
  No abstract at ADS

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Title: A Close Look at the Coronal Density of Procyon
Authors: Schmitt, J. H. M. M.; Drake, J. J.; Haisch, B. M.; Stern,
   R. A.
1996ApJ...467..841S    Altcode:
  We derive the coronal density of the nearby star Procyon, using an
  observation with the short- and medium-wavelength spectrometers on board
  the Extreme-Ultraviolet Explorer satellite (EUVE). Specifically, we have
  identified density-sensitive ratios in lines due to iron in ionization
  stages Fe X to Fe XIV, which have been detected in our EUVE spectra. We
  present these observations and analyze these line ratios, paying careful
  attention to line blends or contamination from other extreme-ultraviolet
  (EUV) lines. We show that all the available density-sensitive
  iron line diagnostics are consistent with the interpretation that
  the overall coronal output of Procyon is dominated by regions with a
  coronal density very much resembling densities typically found in active
  regions on the Sun. We estimate that the corona of Procyon is dominated
  by material at a temperature T<SUB>cor</SUB> ∼ 10<SUP>6.2</SUP> K,
  with no significant amount of material above T ∼ 10<SUP>6.8</SUP>
  K; the characteristic density is n<SUB>e</SUB> ∼ 3 x 10<SUP>9</SUP>
  cm<SUP>-3</SUP> the emission measure is EM ∼ 4.5 × 10<SUP>50</SUP>
  cm<SUP>-3</SUP>. We infer a (visible) volume of V<SUB>tot</SUB> ∼ 5
  x 10<SUP>31</SUP> cm<SUP>-3</SUP> assuming the X-ray emission to arise
  from plasma magnetically confined in loops, we deduce that such loops
  have an average height of h ∼ 2 x 10<SUP>9</SUP> cm and cover about
  20% of the stellar surface. Because of the high coronal density and
  the lack of emission measure substantially below T ∼ 10<SUP>6</SUP>
  K, we conclude also that it is unlikely that there exists a cooler,
  acoustically heated subcorona.

---------------------------------------------------------
Title: Flare energetics: analysis of a large flare on YZ Canis
    Minoris observed simultaneously in the ultraviolet, optical and radio.
Authors: van den Oord, G. H. J.; Doyle, J. G.; Rodono, M.; Gary,
   D. E.; Henry, G. W.; Byrne, P. B.; Linsky, J. L.; Haisch, B. M.;
   Pagano, I.; Leto, G.
1996A&A...310..908V    Altcode:
  The results of coordinated observations of the dMe star YZ CMi
  at optical, UV and radio wavelengths during 3-7 February 1983 are
  presented. YZ CMi showed repeated optical flaring with the largest
  flare having a magnitude of 3.8 in the U-band. This flare coincided
  with an IUE exposure which permits a comparison of the emission measure
  curves of YZ CMi in its flaring and quiescent state. During the flare a
  downward shift of the transition zone is observed while the radiative
  losses in the range 10^4^-10^7^K strongly increase. The optical flare
  is accompanied with a radio flare at 6cm, while at 20cm no emission
  is detected. The flare is interpreted in terms of optically thick
  synchrotron emission. We present a combined interpretation of the
  optical/radio flare and show that the flare can be interpreted within
  the context of solar two-ribbon/white-light flares. Special attention
  is paid to the bombardment of dMe atmospheres by particle beams. We
  show that the characteristic temperature of the heated atmosphere is
  almost independent of the beam flux and lies within the range of solar
  white-light flare temperatures. We also show that it is unlikely that
  stellar flares emit black-body spectra. The fraction of accelerated
  particles, as follows from our combined optical/radio interpretation
  is in good agreement with the fraction determined by two-ribbon flare
  reconnection models.

---------------------------------------------------------
Title: The Extreme-Ultraviolet Spectrum of the Nearby K Dwarf
    ɛ Eridani
Authors: Schmitt, J. H. M. M.; Drake, J. J.; Stern, R. A.; Haisch,
   B. M.
1996ApJ...457..882S    Altcode:
  We present and discuss the extreme-ultraviolet spectrum of the
  nearby K2 dwarf ɛ Eri obtained with the spectrometers onboard the
  Extreme-Ultraviolet Explorer satellite (EUVE). In the EUVE spectrum of
  ɛ Eri we detect emission lines attributable to iron in the ionization
  stages Fe IX to Fe XXI, thus covering a rather large temperature range
  from less than 10<SUP>6</SUP> K to 10<SUP>7</SUP> K. While the lines
  in the lowest and highest ionization stages are relatively weak, the
  strongest lines detected are from Fe XV and Fe XVI, from which we infer
  a peak in the differential emission measure distribution at coronal
  temperatures of log T<SUB>c</SUB> ∼ 6.4; significant emission measure
  is, however, also present at both higher and lower temperatures. This
  is in contrast to both lower activity stars whose EUV spectra are
  dominated by cooler Fe lines in the range 170-180 Å as well as the
  more active stars whose EUV spectra are dominated by hotter Fe lines
  in the range 110-135 Å. Finally, a density determination using line
  ratios of Fe XIII and Fe XIV results in coronal densities for ɛ Eri
  which are similar to solar active region densities.

---------------------------------------------------------
Title: Stellar X-ray Flares
Authors: Haisch, B.
1996mpsa.conf..235H    Altcode: 1996IAUCo.153..235H
  No abstract at ADS

---------------------------------------------------------
Title: A U.S.--Russian Industrial Partnership to Develop a Low-Cost
    IUE-2
Authors: Haisch, B.; Robb, P.; Strong, K.; Stern, R.; Schrijver,
   C. J.; Lemen, J.
1995AAS...187.7204H    Altcode: 1995BAAS...27.1388H
  In 18 years as a NASA observatory IUE has generated more than 10(5)
  spectra and 3000 articles, hosted over 2000 guest observers and launched
  more than 200 doctoral dissertations. On 1 October 1995 science
  operations were transferred entirely to ESA. IUE has been a central
  facility in many multiwavelength programs. It has also supported
  HST by carrying out projects that require more dedicated time than
  HST can accomodate, including the ability to carry out uninterrupted
  observations. Ready access to the UV spectrum has become a routine part
  of modern astronomical capability, especially with respect to surveying
  classes of objects and monitoring for variability and cycles. A
  feasibility study has been initiated in the Solar and Astrophysics
  Laboratory and the Optical Sciences Laboratory to examine an upgraded
  IUE-2 to be developed in partnership with the Vavilov State Optical
  Institute of St. Petersburg, Russia. The Vavilov Institute is the
  premier space optics facility in the former Soviet Union. The recent
  “swords into plowshares” industrial partnership with Vavilov and
  cost-effective capabilities involving commercial boosters such as LLV-2
  and a version of the Commercial Remote Sensing Satellite (CRSS) bus
  open innovative new opportunities for developing scientific facilities
  in space. We are also investigating the economics of a shared launch on
  the large capacity Proton rocket now operated jointly at the Baikonur
  complex in Kazakhstan by Lockheed Martin, Khrunichev Enterprises and
  NPO Energia. The centerpiece of IUE-2 would be a lightweight, advanced
  techology silicon carbide mirror up to 1.2 m in diameter coupled to
  modern imaging detectors. The Vavilov Institute has developed a robust
  ceramic material of remarkable specific rigidity and thermal stability
  that shows no distortion or hysteresis when thermally cycled between
  cryogenic and room temperatures. Mirrors are routinely polished
  to 0.03 waves in the visible. Spectroscopic capabilities would be
  similar to the current IUE. The CRSS spacecraft provides 10 GBytes
  of onboard data storage. In the interest of cost-savings, a highly
  eccentric Exosat-like elliptical orbit is under consideration to
  provide uninterrupted viewing times of at least 12 hours. This study,
  now underway, will examine innovative ways in which a science-driven
  program can be successfully developed and provided to NASA as a
  purchased commercial product. Inputs are solicited, especially from
  IUE guest observers and potentially interested IUE-2 users.

---------------------------------------------------------
Title: Stellar M-Flares Observed by ASCA on Proxima Centauri
Authors: Haisch, B.; Antunes, M.; Schmitt, J. H. M. M.
1995SPD....26.1307H    Altcode: 1995BAAS...27..988H
  No abstract at ADS

---------------------------------------------------------
Title: The Elemental Composition of the Corona of Procyon: Evidence
    for the Absence of the FIP Effect
Authors: Drake, Jeremy J.; Laming, J. Martin; Widing, Kenneth G.;
   Schmitt, Jurgen H. M. M.; Haisch, Bernard; Bowyer, Stuart
1995Sci...267.1470D    Altcode:
  The chemical composition of the solar corona is not the same as that
  of the underlying photosphere. In the corona, elements with a first
  ionization potential (FIP) of &lt;= 10 electron volts (for example,
  iron, magnesium, silicon, and calcium) are overabundant relative
  to those with an FIP of &gt;= 10 electron volts (for example,
  oxygen, neon, and sulfur) by factors of 3 to 10 with respect to the
  photosphere. The origin of this FIP effect is unknown. The launch
  of the Extreme Ultraviolet Explorer Satellite (EUVE) opened up the
  spectroscopic capability required to determine elemental abundances
  in the coronae of other stars. Spectroscopic observations of the
  corona of the nearby F5 IV star Procyon obtained with EUVE have
  yielded estimates of the relative abundances of high- and low-FIP
  species. The results provide evidence that Procyon, unlike the sun,
  does not exhibit the FIP effect. Whether the sun or Procyon is more
  typical of the general late-type stellar population is of fundamental
  interest to the physics of stellar outer atmospheres and has a bearing
  on the origin of cosmic rays.

---------------------------------------------------------
Title: ASCA observations of X-ray flares on Proxima Centauri
Authors: Antunes, Alex; Haisch, B.; Schmitt, J. H. M. M.
1995AAS...186.2102A    Altcode: 1995BAAS...27..838A
  We present the ASCA observation of several flare events on Proxima
  Centauri during March 18-20 1994. Although the quiescent count rate of
  0.23 cts/sec was too low to unambiguously spot line features, flares
  were clearly distinguished with a higher count rate of approximately
  0.9 cts/sec. These are the first stellar flares observed to overlap
  with ordinary solar flares of class M on the GOES scale (Haisch,
  Antunes and Schmitt, 1995, Science, in press). We compared the
  quiescent data with the flare data, and fit the X-ray emission using
  two-temperature and differential emission measure plasma models. Unlike
  several coronal sources (for example, Algol, AR Lac), the models did
  not require sub-solar abundances. However, abundance determinations
  in the absence of clearly distinguishable lines were uncertain. The
  current results support the premise that the coronal X-ray emission
  is a result of the superposition of many flares.

---------------------------------------------------------
Title: The RIASS Coronathon: Joint X-Ray and Ultraviolet Observations
    of Normal F--K Stars
Authors: Ayres, Thomas R.; Fleming, T. A.; Simon, T.; Haisch, B. M.;
   Brown, A.; Lenz, D.; Wamsteker, W.; de Martino, D.; Gonzalez, C.;
   Bonnell, J.; Mas-Hesse, J. M.; Rosso, C.; Schmitt, J. H. M. M.;
   Truemper, J.; Voges, W.; Pye, J.; Dempsey, R. C.; Linsky, J. L.;
   Guinan, E. F.; Harper, G. M.; Jordan, C.; Montesinos, B. M.; Pagano,
   I.; Rodono, M.
1995ApJS...96..223A    Altcode:
  Between 1990 August and 1991 January the ROSAT/IUE All Sky Survey
  (RIASS) coordinated pointings by the International Ultraviolet Explorer
  (IUE) with the continuous X-ray/EUV mapping by the Roentgensatellit
  (ROSAT). The campaign provided an unprecedented multiwavelength
  view of a wide variety of cosmic sources. We report findings for
  F-K stars, a large proportion of the RIASS targets. Forty-eight of
  our 91 'Coronathon' candidates were observed by the IUE during the
  campaign. For stars missed by the IUE, we supplemented the ROSAT survey
  fluxes with archival UV spectra and/or follow-on observations.

---------------------------------------------------------
Title: Stellar x-ray flares
Authors: Haisch, B.; Uchida, Y.; Kosugi, T.; Hudson, H. S.
1995lock.reptR....H    Altcode:
  What is the importance of stellar X-ray flares to astrophysics, or
  even more, to the world at large? In the case of the Sun, changes in
  solar activity at the two temporal extremes can have quite significant
  consequences. Longterm changes in solar activity, such as the Maunder
  Minimum, can apparently lead to non-negligible alterations of the
  earth's climate. The extreme short term changes are solar flares, the
  most energetic of which can cause communications disruptions, power
  outages and ionizing radiation levels amounting to medical X-ray dosages
  on long commercial flights and even potentially lethal exposures for
  unshielded astronauts. Why does the Sun exhibit such behaviour? Even
  if we had a detailed knowledge of the relevant physical processes on
  the Sun - which we may be on the way to having in hand as evidenced
  by these Proceedings- our understanding would remain incomplete in
  regard to fundamental causation so long as we could not say whether the
  Sun is, in this respect, unique among the stars. This current paper
  discusses the stellar x-ray flare detections and astronomical models
  (quasi-static cooling model and two-ribbon model) that are used to
  observe the x-ray emission.

---------------------------------------------------------
Title: ASCA Observations of Solar-like M-flares on Proxima Centauri
Authors: Haisch, B.; Antunes, A.; Schmitt, J. H. M. M.
1994AAS...185.4505H    Altcode: 1994BAAS...26.1380H
  Stellar flares have been observed in the X-ray for twenty years, but
  the events must be much larger --- by as much as a factor of 10(4)
  --- than even the most energetic on the Sun in order to be detected
  across the enormous distances. While stellar “superflares” are of
  considerable interest, it is equally important to ascertain whether and
  with what frequency commonplace solar-like events occur on stars. This
  is an important test of the working hypothesis that we are dealing with
  scaled-up versions of the same physical phenomenon. The new Japanese
  ASCA satellite has now succeeded in this, observing very typical
  M-class solar-like flares on the next nearest star, Proxima Centauri.

---------------------------------------------------------
Title: A Spectroscopic Measurement of the Coronal Density of Procyon
Authors: Schmitt, J. H. M. M.; Haisch, B. M.; Drake, J. J.
1994Sci...265.1420S    Altcode:
  One of the open key issues in the astrophysics of stellar coronae is the
  determination of their spatial structure and density. From almost all
  previous measurements, one can infer merely the presence of a corona,
  which for the most energetic stellar coronae may exceed the solar x-ray
  output by as much as five orders of magnitude, but no information can be
  obtained on the densities and hence volumes and sizes of the hot x-ray
  emitting material. A direct spectroscopic measurement of the coronal
  density was obtained for the star Procyon with the spectrometer on
  board the Extreme Ultraviolet Explorer satellite; the ratio of two
  Fe XIV lines at 211.32 and 264.79 angstroms was used to determine
  a density of ~4 x 10^9 to 7 x 10^9 electrons per cubic centimeter,
  which is a factor of 2 to 3 higher than typical solar active region
  densities. From this value, we estimate that ~6 percent of the stellar
  surface is covered with ~7 x 10^4 coronal loops.

---------------------------------------------------------
Title: The First Measurement of Stellar Coronal Abundances: The
    Absence of the FIP Effect in the Corona of Procyon
Authors: Drake, J. J.; Laming, J. M.; Widing, K. G.; Schmitt,
   J. H. M. M.; Haisch, B.; Bowyer, S.
1994AAS...184.0522D    Altcode: 1994BAAS...26..866D
  The unique spectroscopic capabilities of the Extreme Ultraviolet
  Explorer satellite (EUVE), with wavelength coverage from 70--760
  Angstroms at a resolution of ~ 1 Angstroms, permit for the first time
  the scrutiny in the extreme ultraviolet wavelength regime of individual
  spectral lines emitted by the coronae of stars other than the Sun. We
  have performed a detailed analysis of the first EUVE spectroscopic
  observation of the nearby F5 IV star Procyon and have identified
  lines of the elements O, Ne, Mg, Si, S, Fe, and Ni. The emission
  measure distribution, derived from line intensities measured from the
  EUVE spectra and based on the most recent atomic data, has yielded
  estimates of the relative abundances of these elements in the corona
  of Procyon. The results indicate a total absence of a fractionation of
  elements by first ionization potential (FIP), contrary to such as is
  observed in the solar corona (the “FIP Effect”). These results are
  discussed, and the potential for future EUVE spectroscopic investigation
  into the new field of stellar coronal abundances is highlighted. This
  work has been supported by NASA contract NAS5-30180.

---------------------------------------------------------
Title: EUVE Spectroscopy of XI UMa; sigma Gem; and Chi {1} ORI
Authors: Mewe, R.; Schrijver, C. J.; Kaastra, J. S.; Alkemade,
   F. J. M.; Haisch, B. M.
1994ASPC...64...41M    Altcode: 1994csss....8...41M
  No abstract at ADS

---------------------------------------------------------
Title: Observing a partly cloudy universe.
Authors: Bowyer, S.; Malina, R.; Haisch, B.
1994S&T....88f..36B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The High-Energy View of the Nearby Star Procyon
Authors: Schmitt, J. H. M. M.; Haisch, B. M.; Drake, J. J.
1994HEAD...26...13S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Impulsive Soft X-ray Bursts on the Flare Star UV Ceti
Authors: Haisch, B.; Schmitt, J. H. M. M.; Barwig, H.
1993AAS...18312303H    Altcode: 1993BAAS...25R1475H
  We report on a new and unexpected impulsive phenomenon during two
  stellar flares simultaneously observed in soft X-rays by the ROSAT
  Observatory and using ground-based, high-speed optical photometry at
  the Wendelstein Observatory in Bavaria, Germany. SXR bursts follow
  the U- and B-band events by approximately 30 s. We concentrate on
  the correlation of the optical and initial SXR bursts. Statistical
  analysis verifies the significance of these events. They may offer
  an unexpected window on the impulsive phase of stellar flares. This
  would be especially timely since the ASCA Observatory has just begun
  its mission and should be capable of observing stellar flares in some
  detail. While the precise physical implications of our observations
  remain unclear, we argue that our data show the signature of X-ray
  emission from the impulsive phase of a stellar flare rather than that
  of a microflare or a compact loop flare. The curious time relationship
  between the optical and SXR bursts may lend support to a gas-dynamic
  model proposed by Katsova and Livshits.

---------------------------------------------------------
Title: Implications of Initial Results from the EUVE Observatory
    for the FUSE EUV Spectrometer and a Possible EUVE Extended Mission
Authors: Malina, R. F.; Finley, D.; Warren, J.; Fruscione, A.;
   Edelstein, J.; Haisch, B.
1993AAS...183.1716M    Altcode: 1993BAAS...25.1320M
  We summarize the initial scientific results from the Extreme
  Ultraviolet Explorer (EUVE) observatory all-sky survey and Guest
  Observer Programs. The initial results include the first EUVE catalog
  (Bowyer et al. 1993) which reports characteristics of 410 extreme
  ultraviolet (EUV) sources and the spectroscopic observations by
  guest observers of large numbers of classes of different kinds of EUV
  sources. We assess the implication of these initial results on the
  scientific objectives of the EUV spectrometer on NASA's Far Ultraviolet
  Spectroscopic Explorer (FUSE). The FUSE EUV spectrometer will have an
  order of magnitude more collecting area than the EUVE spectrometer and a
  resolving power several times higher. Current NASA planning anticipates
  a turn off of the EUVE observatory following the third year of the
  EUVE Guest Observer Program in 1996. A proposal is currently being
  prepared for NASA, in collaboration with the EUVE Users Committee,
  for an extension of the EUVE mission. Based on the EUVE results, we
  raise issues which must be taken into account in designing a science
  program for a possible extension of the EUVE mission such as the
  total number of EUV sources observable spectroscopically by EUVE. We
  distinguish between the science return from an EUVE extended mission
  and from the EUV spectrometer on FUSE given the different capabilities
  of the two instruments. We discuss in detail the types of scientific
  investigations that can be expected for cool stars, white dwarfs,
  extragalactic objects and cataclysmic variables. The work reported
  here was funded by NASA Contract NAS5--29298.

---------------------------------------------------------
Title: The Extreme Ultraviolet Explorer mission: overview and
    initial results.
Authors: Haisch, B.; Bowyer, S.; Malina, R. F.
1993JBIS...46R.331H    Altcode:
  The successful launch of the NASA Extreme Ultraviolet Explorer on
  June 7, 1992, is the culmination of nearly 30 years of effort at the
  University of California at Berkeley to open up the field of extreme
  ultraviolet astronomy. The authors present a brief introduction to
  this field and an overview of the satellite instrumentation.

---------------------------------------------------------
Title: The Extreme Ultraviolet Explorer mission - Overview and
    initial results
Authors: Haisch, B.; Bowyer, S.; Malina, R. F.
1993JBIS...46Q.331H    Altcode:
  The history of extreme ultraviolet (EUV) astronomy is briefly
  reviewed, and an overview of the Extreme Ultraviolet Explorer
  mission, launched into a near-earth (550 km) orbit on June 7, 1992,
  is presented. First, the principal objective of the mission are
  summarized. The instrumentation and operation of the mission are
  then described, with particular attention given to the sky survey
  instruments, the deep survey instrument, and the spectrometers. The
  discussion also covers the current view of the interstellar medium,
  early results from the mission, and future prospects for EUV astronomy.

---------------------------------------------------------
Title: The EUV Coronal Spectrum of chi (1) ORI (HR 2047, G0 V)
Authors: Haisch, B.; Drake, J.; Schmitt, J. H. M. M.
1993AAS...182.4115H    Altcode: 1993BAAS...25..862H
  We have carried out an 80 ks extreme ultraviolet observation of the
  active solar-like star chi (1) Ori using the Extreme Ultraviolet
  Explorer (EUVE) spectrograph. Based on its chromospheric activity
  level, this star appears to be quite young (see Haisch and Basri,
  1985, Ap. J. Suppl., 58, 179). Its X-ray luminosity as measured by
  the Einstein IPC (log L_x = 28.8) and the ROSAT PSPC (log L_x = 29.1)
  makes it a factor of ten more active than the Sun at solar maximum. We
  present the first EUV spectrum of an active solar-like star.

---------------------------------------------------------
Title: ROSAT observations of the stellar coronal dividing line.
Authors: Haisch, B.; Schmitt, J. H. M. M.
1993uxrs.conf..547H    Altcode: 1993uxsa.conf..547H
  The authors present an update on the results of the ROSAT X-ray All-Sky
  Survey observations of stellar sources presented by Haisch, Schmitt
  and Rosso (1991). In that paper the presence of a coronal dividing
  line in the H-R diagram at approximately spectral type K3 II to K3
  IV was established by the clear difference in distribution of the 65
  ROSAT detections vs. the 868 non-detections of BSC stars in the 70
  percent-complete survey. The remaining 30 percent of the survey has
  now been processed resulting in 31 additional detections of stellar
  coronae, all of which lie to the left of the dividing line.

---------------------------------------------------------
Title: The Stellar Coronal Dividing Line
Authors: Haisch, B.; Schmitt, J. H. M. M.
1992AAS...181.2308H    Altcode: 1992BAAS...24.1159H
  No abstract at ADS

---------------------------------------------------------
Title: Coordinated Ginga, IUE, and VLA Observations of Stellar
    Activity in sigma 2 Coronae Borealis
Authors: Stern, R. A.; Uchida, Y.; Walter, F.; Vilhu, O.; Hannikainen,
   D.; Brown, A.; Veale, A.; Haisch, B. M.
1992ApJ...391..760S    Altcode:
  Observations of the active cool star binary system Sigma(2) Corona
  Borealis with the Large Area Counters on the Ginga X-ray satellite
  over 2.5 d, or about two orbital periods, are reported. Throughout
  the observations, Sigma(2) CrB exhibited X-ray variability on time
  scales ranging from tens of minutes to hours. The X-ray light curve
  shows evidence of flaring during the course of the observations. The
  summed X-ray pulse height spectrum from flaring events compared
  with similar spectra from quiescent periods indicates an increase in
  coronal temperature. Periodogram analysis of the entire X-ray light
  curve shows a possible periodicity at about 0.40-0.44 d, with no strong
  signal at the orbital period or 1/2 of the orbital period. Coordinated
  multiwavelength observations of IUE and the VLA indicate both UV and
  microwave flaring during one X-ray outburst. The quiescent microwave
  spectrum is not consistent with a thermal gyrosynchrotron process;
  nonthermal gyrosynchrotron radiation is argued to be the most likely
  emission process.

---------------------------------------------------------
Title: IUE/ROSAT Observations of Proxim Centauri Flares
Authors: Haisch, Bernard
1992iue..prop.4332H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronal Heating and the Dividing Line (With 2 Figures)
Authors: Haisch, B.
1991mcch.conf..225H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Recent Advances in Extreme Ultraviolet Astronomy with
    Multilayers
Authors: Haisch, B. M.; Whittemore, T. E.; Rottman, G. J.
1991eua..coll..368H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Rotational modulation and flares on RS Canum Venaticorum and
    BY Draconis-type stars. XV. Observations of Proxima Centauri and
    solar calibration data.
Authors: Haisch, B. M.; Butler, C. J.; Foing, B.; Rodono, M.; Giampapa,
   M. S.
1990A&A...232..387H    Altcode:
  Results are reported from simultaneous Exosat and IUE observations
  of flaring in Proxima Cen on March 2, 1985. The data are presented in
  extensive tables and sample spectra and discussed in detail. The peak
  emission of the soft-X-ray flare is found to be about 3 x 10 to the 27th
  erg/sec, with energy about 3 x 10 to the 30th erg and an associated
  increase in Mg II flux to 17,000-67,000 erg/sq cm sec, or about an
  order of magnitude lower than the solar value. The presence of flare-
  and microflare-related processes heating the corona is inferred.

---------------------------------------------------------
Title: Rotational modulation and flares on RS Canum Venaticorum and
    BY Draconis-type stars. XIV. Phasen eclipse and flare observations
    of YY Geminorum by EXOSAT and IUE.
Authors: Haisch, B. M.; Schmitt, J. H. M. M.; Rodono, M.; Gibson, D. M.
1990A&A...230..419H    Altcode:
  The eclipsing spectroscopic binary YY Geminorum has been observed
  at optical, ultraviolet, and X-ray wavelengths for rotational
  modulation, eclipse variability, and flaring. The epoch T(phi = 0) =
  JD 2425698.3561, and the phase P = 0.81428224 d. The quiescent level
  of Mg II emission is remarkably steady during the three-year observing
  interval, with F(Mg II) roughly 3.6 x 10 to the -12th erg/sq cm/s. Both
  stars appear to have identical Mg II surface fluxes, with F roughly
  1.8 x 10 to the 6th erg/sq cm/s. Both stars appear to be covered
  with evenly distributed Mg II emitting regions consistent with the
  proposition of Doyle (1987) that saturation of the Mg II lines occurs
  for stars having P less than 4 d, implying that such stars are entirely
  covered by plage. The transition region lines show significantly more
  rotational modulation and/or secular variability than Mg II. Both Mg II
  and the transition region lines show preflare and postflare enhancement.

---------------------------------------------------------
Title: Co-Ordinated GINGA IUE and VLA Observations of Flaring Activity
    in SIGMA-2 CRB
Authors: Stern, R. A.; Haisch, B. M.; Uchida, Y.; Walter, F.; Veale,
   A.; Brown, A.; Vilhu, O.; Hannikainen, D.
1990ASPC....9..227S    Altcode: 1990csss....6..227S
  The RS CVn system sigma-squared CrB was observed by the Ginga
  X-ray satellite for a period of 2.5 days, or approximately 2 binary
  orbits. Sigma-squared CrB exhibited almost continuous X-ray variability
  on time scales ranging from minutes to days, including several
  'flare-like' episodes with increased coronal temperature. The average
  count rate was 4.2 +/- 1.2 cts/s (1.7-11.0 keV) corresponding to L(x)
  of about 10 to the 29.6th erg/s (2-10 keV). Coordinated observations
  with IUE and the VLA indicate microwave and ultraviolet flaring
  associated with one X-ray flare.

---------------------------------------------------------
Title: The X-Ray Emission of Late Type Evolved Stars
Authors: Maggio, A.; Vaiana, G. S.; Haisch, B. M.; Stern, R. A.;
   Harnden, F. R., Jr.; Rosner, R.
1990ixra.conf..233M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Einstein Observatory Magnitude-limited X-Ray Survey of
    Late-Type Giant and Supergiant Stars
Authors: Maggio, A.; Vaiana, G. S.; Haisch, B. M.; Stern, R. A.;
   Bookbinder, J.; Harnden, F. R., Jr.; Rosner, R.
1990ApJ...348..253M    Altcode:
  Results are presented of an extensive X-ray survey of 380 giant and
  supergiant stars of spectral types from F to M, carried out with
  the Einstein Observatory. It was found that the observed F giants
  or subgiants (slightly evolved stars with a mass M less than about 2
  solar masses) are X-ray emitters at the same level of main-sequence
  stars of similar spectral type. The G giants show a range of emissions
  more than 3 orders of magnitude wide; some single G giants exist with
  X-ray luminosities comparable to RS CVn systems, while some nearby
  large G giants have upper limits on the X-ray emission below typical
  solar values. The K giants have an observed X-ray emission level
  significantly lower than F and F giants. None of the 29 M giants were
  detected, except for one spectroscopic binary.

---------------------------------------------------------
Title: GINGA Observations of a Long Duration X-Ray Flare in the
    Algol System
Authors: Stern, R. A.; Haisch, B. M.; Nagase, F.; Uchida, Y.;
   Tsuneta, S.
1990ASPC....9..224S    Altcode: 1990csss....6..224S
  Algol was observed by the Ginga X-ray satellite for about 2 days in
  January 1989, including both the primary and most of the secondary
  optical eclipses. No evidence for X-ray eclipses was seen. A large
  flare lasting over 12 h was detected prior to and during secondary
  eclipse. The flare began with a peak temperature of about 69 MK,
  gradually decaying to about 36 MK. Variable Fe line emission at 6.7
  keV ws observed. The Fe line equivalent width is in clear disagreement
  with theoretical predictions for an optically thin plasma.

---------------------------------------------------------
Title: Ginga Observations of a Long-Duration X-ray Flare in Algol
Authors: Stern, R. A.; Haisch, B. M.; Nagase, F.; Uchida, Y.;
   Tsuneta, S.
1989BAAS...21.1205S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A relation between Balmer and soft X-ray emission in flares
Authors: Haisch, B. M.
1989A&A...219..317H    Altcode:
  Data are presented on 370 solar flares simultaneously observed and
  classified in H-alpha and in the GOES (1-8 A) soft X-ray band. SMM
  observations corroborate the association of the GOES and the H-alpha
  events in all cases. These flares are used to examine the correlation
  proposed recently by Butler, Rodono and Foing (1988).

---------------------------------------------------------
Title: Simultaneous multi-wavelength observations of an intense
    flare on AD Leonis.
Authors: Rodono', M.; Houdebine, E. R.; Catalano, S.; Foing, B.;
   Butler, C. J.; Scaltriti, F.; Cutispoto, G.; Gary, D. E.; Gibson,
   D. M.; Haisch, B. M.
1989sasf.confP..53R    Altcode: 1989IAUCo.104P..53R; 1988sasf.conf...53R
  The authors report on the first successful coordinated observations
  of stellar flares carried out on March 28, 1984 simultaneously over
  a wide range of wavelengths, from UV to microwaves, using the IUE
  satellite, three ESO telescopes at La Silla (Chile) and the VLA at
  Socorro (NM, USA).

---------------------------------------------------------
Title: Solar and stellar flares
Authors: Haisch, B. M.; Rodono, M.
1989SoPh..121.....H    Altcode: 1989IAUCo.104.....H
  Various papers on solar physics are presented. Individual topics
  addressed include: electron beam as origin of white-light solar flares,
  solar flare diagnostic, multiwavelength observations of stellar flares,
  impulsive phase of solar flares, electron acceleration in solar
  flares, models of flaring loops, stellar flare spectral diagnostics,
  preflare activity, radio emission from stellar flares, mass motions
  associated with solar flares, importance of solar white-light flares,
  hydrodynamic models of solar and stellar flares, long-duration solar
  and stellar flares, magnetic equilibria and instabilities, stellar
  flare statistics, role of eruption in solar flares, gradual phase
  in solar flares, polarimetry of stellar active regions and flares,
  particle acceleration in solar flares, and cyclotron lines in the
  spectra of solar flares and solar active regions.

---------------------------------------------------------
Title: The X-ray Emission of Late-Type Giant and Supergiant Stars:
    Results of the Einstein Observatory Magnitude-Limited X-ray Survey
Authors: Maggio, A.; Vaiana, G. S.; Haisch, B. M.; Stern, R. A.;
   Harnden, F. R.; Rosner, R.
1988feta.conf...12M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: EUV and XUV Observations of the Solar Corona made in
    Conjunction with the Total Solar Eclipse of 1988 March 17/18
Authors: Rottman, G. J.; Hassler, D. M.; Jones, M. D.; Orrall, F. Q.;
   Haisch, B. M.; Whittemore, T. E.
1988BAAS...20..703R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Soft X-ray images of the solar corona using normal incidence
    optics.
Authors: Bruner, M. E.; Haisch, B. M.; Brown, W. A.; Acton, L. W.;
   Underwood, J. H.
1988JPhys..49..115B    Altcode: 1988IAUCo.102..115B
  A solar coronal loop system has been photographed in soft X-rays using
  a normal incidence telescope based on multilayer mirror technology. The
  image was recorded during a rocket flight on 1985 October 25, and was
  dominated by emission lines arising from the Si XII spectrum. The
  rocket also carried a high resolution soft X-ray spectrograph that
  confirmed the presence of Si XII line radiation in the source.

---------------------------------------------------------
Title: A multilayer X-ray mirror for solar photometric imaging flown
    on a sounding rocket.
Authors: Haisch, B. M.; Whittemore, T. E.; Joki, E. G.; Brookover,
   W. J.; Rottman, G. J.
1988SPIE..982...38H    Altcode: 1988xia..conf...38H
  The authors discuss the flight of a multilayer-coated mirror on a
  sounding rocket experiment on March 17, 1988, which was used to obtain
  photometric images of the Sun just prior to solar eclipse. Eight
  full-disk images of the Sun were obtained by this XUV imager. The
  images are of excellent quality and are being anlyzed together with
  coordinated ground-based, eclipse coronagraph observations and radio
  maps taken at the VLA and Greenbank.

---------------------------------------------------------
Title: Coordinated Multiband Space and Groundbased Observations of
    Surface Structures and Flares on Late Type Stars
Authors: Foing, B.; Butler, C. J.; Haisch, B. M.; Linsky, J. L.;
   Rodono, M.
1988copa.conf..197F    Altcode:
  The authors discuss the need to coordinate future synoptic observations
  at all accessible wavelengths for these objects which are highly
  variable on all timescales from seconds to years.

---------------------------------------------------------
Title: X-Ray Photographs of a Solar Active Region with a Multilayer
    Telescope at Normal Incidence
Authors: Underwood, J. H.; Bruner, M. E.; Haisch, B. M.; Brown, W. A.;
   Acton, L. W.
1987Sci...238...61U    Altcode:
  An astronomical photograph was obtained with a multilayer x-ray
  telescope. A 4-centimeter tungsten-carbon multilayer mirror was flown
  as part of an experimental solar rocket payload, and successful
  images were taken of the sun at normal incidence at a wavelength
  of 44 angstroms. Coronal Si-XII emission from an active region was
  recorded on film; as expected, the structure is very similar to that
  observed at O-VIII wavelengths by the Solar Maximum Mission flat crystal
  spectrometer at the same time. The small, simple optical system used
  in this experiment appears to have achieved a resolution of 5 to 10
  arc seconds.

---------------------------------------------------------
Title: Rotational modulation and flares on RS CVn and BY Dra-type
    stars. V. EXOSAT and IUE observations of a flare on EQ Pegasi.
Authors: Haisch, B. M.; Butler, C. J.; Doyle, J. G.; Rodono, M.
1987A&A...181...96H    Altcode:
  Time-trailed UV spectra and a soft X-ray lightcurve were obtained
  during a flare on the binary dMe star EQ Peg AB. On the basis of solar
  flare Mg II surface fluxes and an about 70-percent enhancement in
  the disk-integrated flux during the flare on EQ Peg, it is estimated
  that the chromospheric flare covered about 1.5 percent of the stellar
  surface. The size scale is estimated to be comparable to that of a solar
  two-ribbon flare. This unusual flare is noted to exhibit a low-energy
  soft X-ray rise phase which is longer than that of most flares; it
  is longer than the decay phase and peaks much later than the medium
  energy light curve. Evidence of variable Fe II emission and variable
  continuum emission in select UV bands during the flare is noted.

---------------------------------------------------------
Title: Very high resolution UV and X-ray spectroscopy and imagery
    of solar active regions
Authors: Bruner, M.; Brown, W. A.; Haisch, B. M.
1987lock.rept.....B    Altcode:
  A scientific investigation of the physics of the solar atmosphere,
  which uses the techniques of high resolution soft X-ray spectroscopy
  and high resolution UV imagery, is described. The experiments were
  conducted during a series of three sounding rocket flights. All three
  flights yielded excellent images in the UV range, showing unprecedented
  spatial resolution. The second flight recorded the X-ray spectrum of a
  solar flare, and the third that of an active region. A normal incidence
  multi-layer mirror was used during the third flight to make the first
  astronomical X-ray observations using this new technique.

---------------------------------------------------------
Title: Simultaneous X-ray and optical monitoring of the flare star
    YZ CMi.
Authors: Doyle, J. G.; Butler, C. J.; Haisch, B. M.; Rodono, M.
1986MNRAS.223P...1D    Altcode:
  Broad-band photometric observations of YZ CMi show a 1.2 mag U-band
  flare, however, simultaneous X-ray observations from EXOSAT show no
  detectable increase. It is suggested that the event could have occurred
  low down in a part of the chromosphere, which may not have been coupled
  to the transition region and corona via magnetic fields. However,
  a more plausible explanation may have been absorption of the X-rays
  by an over-lying dense prominence. Several short-lived enhancements
  (micro-flares) were detected in both the Johnson U-band and the Balmer
  emission lines.

---------------------------------------------------------
Title: Variability in Active Region Coronal Loops
Authors: Haisch, B. M.
1986BAAS...18Q.901H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Local Distribution of Interstellar Matter Derived from
    (B-V) Colors of Bright Stars
Authors: Davidson, G. T.; Claflin, E. S.; Haisch, B. M.
1986BAAS...18.1036D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Dividing Line for Stellar Coronae
Authors: Antiochos, S. K.; Haisch, B. M.; Stern, R. A.
1986ApJ...307L..55A    Altcode:
  The authors describe a possible explanation for the observation that
  late-type stars falling in a certain region of the H-R diagram exhibit
  no X-ray emission and, hence, appear not to have coronae. The basic
  idea of the authors' model is that due to the low surface gravity
  that characterizes the stars without X-ray emission, a hot (T &gt;
  10<SUP>6</SUP>K) corona is thermally unstable and spontaneously
  cools down to chromospheric temperatures. The key parameter that
  determines the outer atmospheric structure is shown to be the ratio
  of the gravitational scale height of plasma at T = 10<SUP>5</SUP>K to
  the maximum height of closed magnetic field lines in the corona.

---------------------------------------------------------
Title: Coordinated Exosat and spectroscopic observations of flare
    stars and coronal heating
Authors: Butler, C. J.; Rodono, M.; Foing, B. H.; Haisch, B. M.
1986Natur.321..679B    Altcode:
  The X-ray flux of dMe stars is thought to arise from two distinct
  mechanisms, one involving a continuous `quiescent' emission from a
  high-temperature plasma and the other involving the dramatic flare
  events which have long been known to occur on these stars. We present
  here some results of simultaneous monitoring of the two flare stars, UV
  Ceti and EQ Peg, with Exosat and ground-based optical spectroscopy. We
  observe short-timescale variability in the 0.1-2-keV emission from both
  these objects and, in the case of UV Ceti, find a strong correlation
  between the soft X-ray and Hγ fluctuations. The implication is that
  much of the low-level X-ray flux previously considered `quiescent'
  probably originates from small flare events.

---------------------------------------------------------
Title: Non-Potential Features Observed in the Magnetic Field of an
    Active Region
Authors: Gary, G. A.; Moore, R. L.; Hagyard, M. J.; Haisch, B. M.
1986BAAS...18..709G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronae on Stars
Authors: Haisch, B. M.
1986IrAJ...17..200H    Altcode:
  Three lines of evidence are noted to point to a flare heating source for
  stellar coronae: a strong correlation between time-averaged flare energy
  release and coronal X-ray luminosity, the high temperature flare-like
  component of the spectral signature of coronal X-ray emission, and the
  observed short time scale variability that indicates continuous flare
  activity. It is presently suggested that flares may represent only
  the extreme high energy tail of a continuous distribution of coronal
  energy release events.

---------------------------------------------------------
Title: Coordinated IUE and ground-based observations of stellar
flares: YZ CMi, Proxima Cen and AD Leo.
Authors: Foing, B. H.; Rodono, M.; Cutispoto, G.; Catalano, S.; Linsky,
   J. L.; Gibson, D. M.; Brown, A.; Haisch, B. M.; Butler, C. J.; Byrne,
   P. B.; Andrews, A. D.; Doyle, J. G.; Gary, D. E.; Henry, G. W.; Russo,
   G.; Vittone, A.; Scaltriti, F.
1986RMxAA..12..213F    Altcode:
  Coordinated observations of stellar flares were obtained with lUE
  and several ground-based facilities in March 1984.The simultaneous
  observations allowed it to cover a wide range of wavelengths from ii5nm
  to 6cm.We intend to study the effect ofthe observed flares at different
  atmospheric heights in order to estimate the energy budget,the time
  scales and the cooling processes.Our observations includetime-resolved
  IUE spectroscopy at SWP(115-195nm) and LWP(190-320nm),optical
  spectroscopy at the ESO 3.6m+IDS (355-440nm),high resolution
  spectroscopy at the ESO 1.4m CAT+CES(653-659nm),narrow band H alpha
  and wide band optical photometry, infrared photometry at 2.2microns
  and microwave observations at 2,6 and 20 cm We present for some
  flare events,among the results,the first detection of infrared flux
  decrease -or "negative flare"-in coincidence with the flux increase
  at the other wavelengths:the broadening and changes of the Balmer H
  lines,He and high excitation lines;the appearance of higher members
  of the Balmer serie;the enhancements of Mg II doublet and Fe II blend
  (260nm);and the flare detection at 2cm and 6cm

---------------------------------------------------------
Title: A Comparison of Photospheric Electric Current and Ultraviolet
    and X-Ray Emission in a Solar Active Region
Authors: Haisch, B. M.; Bruner, M. E.; Hagyard, M. J.; Bonnet, R. M.
1986ApJ...300..428H    Altcode:
  This paper presents an extensive set of coordinated observations
  of a solar active region, taking into account spectroheliograms
  obtained with the aid of the Solar Maximum Mission (SMM) Ultraviolet
  Spectrometer Polarimeter (UVSP) instrument, SMM soft X-ray polychromator
  (XRP) raster maps, and high spatial resolution ultraviolet images of
  the sun in Lyman-alpha and in the 1600 A continuum. These data span
  together the upper solar atmosphere from the temperature minimum to
  the corona. The data are compared to maps of the inferred photospheric
  electric current derived from the Marshall Space Flight Center (MSFC)
  vector magnetograph observations. Some empirical correlation is found
  between regions of inferred electric current density and the brightest
  features in the ultraviolet continuum and to a lesser extent those
  seen in Lyman-alpha within an active region.

---------------------------------------------------------
Title: Flares: the solar-stellar perspective and opportunities.
Authors: Haisch, B. M.
1986RALR...85..224H    Altcode:
  The author outlines eight specific areas in which fundamental concepts
  of flare physics will almost certainly be tested and refined via
  a solar-stellar approach. 1. Electron beam versus superthermal
  heating of the lower flare atmosphere. 2. The chromospheric and
  photospheric response: white-light flaring. 3. Microflaring and the
  heating of coronae and the driving of winds. 4. Flare rates and power
  spectra. 5. Mass motions. 6. Elemental abundance anomalies during
  flares. 7. Periodicities: links to the interior structure of the Sun
  and stars. 8. Flaring on other than dMe stars.

---------------------------------------------------------
Title: X-Ray Resonance Scattering in a Spherically Symmetric
    Coronal Model
Authors: Haisch, B. M.; Claflin, E. S.
1985SoPh...99..101H    Altcode:
  In the solar corona the opacities of some of the prominent X-ray
  emission lines are on the order of τ ≈ 1 over typical coronal
  path lengths. We present and discuss a particular solution of
  the radiative transfer problem involving an extended, spherically
  symmetric coronal shell radiating isotropic, homogeneous emission
  in which single-scattering also takes place. Within the context of
  this simplified model we find that scattered radiation is an important
  contribution to the total emergent resonance line flux and that for the
  He-like family of resonance (r), intercombination (i), and forbidden
  (f) lines, the ratio G=(f + i)/r would decrease as a function of
  optical depth for disk-center emission in an extended spherically
  symmetric corona.

---------------------------------------------------------
Title: IUE spectra of GO V-G5 V solar-type stars.
Authors: Haisch, B. M.; Basri, G.
1985ApJS...58..179H    Altcode:
  An atlas of IUE short-wavelength spectra for a set of 14 bright G0
  V-G5 V stars are presented, and it is shown that these manifest a
  range of qualitatively different chromospheric and transition region
  spectra and significant differences in radiative flux originating at
  the temperature minimum level. A comprehensive survey of observational
  data and physical parameters of these stars has been performed, and
  tabular summaries of the data are presented. It is concluded that
  the UV continuum longward of about 1600 A is a diagnostic of the
  temperature minimum. A considerable range of minimum temperature for
  stars of similar effective temperature and spectral type is found. The
  temperature minimum of the sun is highly structured on spatial scales
  of about one arcsec.

---------------------------------------------------------
Title: Peculiar emission lines in the spectrum of the flare star YZ
    Canis Minoris.
Authors: Haisch, B. M.; Glampapa, M. S.
1985PASP...97..340H    Altcode:
  During a series of spectral scans in search of flares on the dMe
  star YZ CMi the authors observed prominent chromospheric emission
  lines of Hγ λ4340, Hδ λ4100, Ca II H λ3968 blended with Hɛ
  λ3970, Ca II K λ3934, and Hζ λ3889. During one five-minute scan
  the authors recorded the following peculiar transient phenomena:
  (1) the appearance of an exceptionally strong line at ≡λ4007; (2)
  the simultaneous appearance of another prominent feature at ≡λ4276;
  and (3) a change in the ratio of (Ca II H+Hɛ)/Ca II K. The authors
  discuss the possible origin of this unusual transient spectrum.

---------------------------------------------------------
Title: An analysis of scattered light in low dispersion IUE spectra.
Authors: Basri, G.; Clarke, J. T.; Haisch, B. M.
1985A&A...144..161B    Altcode:
  A detailed numerical simulation of light scattering from the
  low-resolution grating in the short wavelength spectrograph of the
  IUE Observatory was developed, in order to quantitatively analyze the
  effects of scattering on both continuum and line emission spectra. It
  is found that: (1) the redistribution of light by grating scattering
  did not appreciably alter either the shape or the absolute flux level
  of continuum spectra for A-F stars; (2) late-type stellar continua
  showed a tendency to flatten when observed in scattered light toward
  the shorter wavelengths; and (3) the effect of grating scattering
  on emission lines is to decrease measured line intensities by an
  increasing percentage toward the shorter wavelengths. The spectra
  obtained from scattering experiments for solar-type and late type
  stars are reproduced in graphic form.

---------------------------------------------------------
Title: Coordinated Multiband Observations of Stellar Flares
Authors: Rodono, M.; Foing, B. H.; Linsky, J. L.; Butler, J. C.;
   Haisch, B. M.; Gary, D. E.; Gibson, D. M.
1985Msngr..39....9R    Altcode:
  The March 28, 1984 flare of AD Leo is characterized on the basis of
  observations obtained over the spectral range from 200 nm to 20 cm using
  the IUE, the VLA, and four ESO telescopes as part of a coordinated
  multiband international campaign. The data are presented graphically
  and discussed, with consideration of faint negative K-band events
  observed simultaneously with the optical flare; an H-alpha precursor
  with longer energy-release relaxation than in the U continuum; and
  remarkably enhanced UV continuum, Mg II doublet, and 260-nm Fe II
  blend during the last secondary optical peak.

---------------------------------------------------------
Title: Soft X-ray polychromator for the Solar Maximum Mission
Authors: Haisch, B. M.; Levay, M.; Stern, R. A.; Strong, K. T.;
   Wolfson, C. J.; Acton, L. W.
1984lock.rept.....H    Altcode:
  The XRP was designed to measure the following temporal and spatial
  properties of the active and flaring Sun: electron temperature,
  departures from steady state, ion kinetic temperatures, and electron
  density. The Bent Crystal Spectrometer (BCS) is capable of measuring
  the broadening and blue shifts often observed in the impulsive phase of
  flares. The six simultaneous line fluxes indicative of six different
  temperatures of formation observable by the Flat Crystal Spectrometer
  (FCS) allows the derivation of the differential emission measure of
  the plasma at each raster point. During the operational periods of the
  XRP hundreds of flares of C-level (GOES classification) were observed
  and brighter in both the FCS and BCS, including 5 X-flares. Associated
  theoretical work in atomic physics, stimulated in part by the promise
  of XRP measurements, has benefitted from the experimental data on
  solar plasmas which the XRP has provided in abundance.

---------------------------------------------------------
Title: X-ray, Ultraviolet, Optical and Magnetic Structure in and
    near an Active Region
Authors: Haisch, B. M.; Tarbell, T. D.; Bruner, M. E.; Acton, L. W.;
   Bonnet, R. M.; Hagyard, M. J.
1984BAAS...16Q1002H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coordinated IUE and ground-based observations of active stars:
    flare events on YZ CMi, V1005 Ori, AD Leo and AR Lac.
Authors: Rodonò, M.; Cutispoto, G.; Catalano, S.; Linsky, J. L.;
   Gibson, D. M.; Brown, A.; Haisch, B. M.; Butler, C. J.; Byrne, P. B.;
   Andrews, A. D.; Doyle, J. G.; Gary, D. E.; Henry, G. W.; Russo, G.;
   Vittone, A.; Scaltriti, F.; Foing, B.
1984ESASP.218..247R    Altcode: 1984iue..conf..247R
  Observations of stellar flares were obtained with IUE and ground-based
  facilities simultaneously over a wide range of wavelengths in order
  to study the effect of the flare radiation at different atmospheric
  levels. Observations include time-resolved IUE and optical spectroscopy,
  narrow and wide-band optical photometry, IR photometry, and microwave
  observations. Results include detection of IR flux decrease, or negative
  flare, in coincidence with flux increase at all other wavelengths.

---------------------------------------------------------
Title: Normal incidence multilayer mirrors for extreme ultraviolet
    astronomy.
Authors: Stern, R. A.; Haisch, B. M.; Joki, E. G.; Catura, R. C.
1984SPIE..445..347S    Altcode:
  Sputtered multilayer coatings allow the use of normal incidence optics
  in the extreme ultraviolet (EUV) region below 500 Å. Multilayer
  mirrors can be tailored to provide images at strong EUV lines in the
  sun and stars, in many cases making more efficient use of the telescope
  aperture than grazing incidence optics. Current efforts in the design,
  fabrication, and testing of EUV multilayer mirrors are discussed.

---------------------------------------------------------
Title: Creation of photometric star catalogs using UBV data and
    model stellar atmospheres.
Authors: Haisch, B. M.; Johnson, H. M.; Davidson, G. T.
1983JAnSc..31..473H    Altcode:
  The creation of star catalogs for any sensor system is accomplished
  with the use of observations in the UBV system in conjunction with
  the theoretical predictions of stellar fluxes derived from models of
  stellar atmospheres. A comparison of data on eight of the principal
  photometric systems currently in use shows that the Johnson UBV system
  and its extension clearly provides the most extensive data base, though
  the uvby system is better suited for estimating the stellar parameters
  of temperature, gravity, and abundance. The absolute calibration of
  the UBV system is discussed in detail. It is shown that for distant
  (reddened) stars, the spectral energy distribution function is affected
  by wavelength-dependent scattering and absorption. New updated tables
  for effective temperature, gravity, and (B - V) color are presented
  for all normal MK-type stars. Also, tables and prescriptions are
  given for identifying many special and peculiar types of stars by
  equivalent MK-types.

---------------------------------------------------------
Title: IUE Observations of a Peculiar Flare Event on the dM0. 5e
    Star G1 182
Authors: Haisch, B. M.; Linsky, J. L.; Bornmann, P. L.; Rodono, M.
1983BAAS...15..948H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Transport and Containment of Plasmas Particles and Energy
    Within Flares
Authors: Acton, L. W.; Brown, W. A.; Bruner, M. E. C.; Haisch, B. M.;
   Strong, K. T.
1983SoPh...86...79A    Altcode:
  Results from the analysis of flares observed by the Solar Maximum
  Mission (SMM) and a recent rocket experiment are discussed. We
  find evidence for primary energy release in the corona through the
  interaction of magnetic structures, particle and plasma transport
  into more than a single magnetic structure at the time of a flare
  and a complex and changing magnetic topology during the course of a
  flare. The rocket data are examined for constraints on flare cooling,
  within the context of simple loop models. These results form a basis
  for comments on the limitations of simple loop models for flares.

---------------------------------------------------------
Title: Coordinated Einstein and IUE observations of a disparitions
    brusques type flare event and quiescent emission from Proxima
    Centauri.
Authors: Haisch, B. M.; Linsky, J. L.; Bornmann, P. L.; Stencel,
   R. E.; Antiochos, S. K.; Golub, L.; Vaiana, G. S.
1983ApJ...267..280H    Altcode:
  The Einstein Imaging Particle Counter observed a major X-ray flare
  in its entirety during a 5-hr period of simultaneous observations,
  with the IUE, of the dM5e flare star Proxima Centauri in August,
  1980. The detailed X-ray light curve, temperature determinations
  during various intervals, and UV line fluxes obtained before, during,
  and after the flare indirectly indicate a 'two-ribbon flare' prominence
  eruption. The calculated ratio of coronal to bolometric luminosity for
  the event is about 100 times the solar ratio. The Proxima Cen corona
  is analyzed in the context of static loop models, in light of which
  it is concluded that less than 6% of the stellar surface seems to be
  covered by X-ray emitting active regions.

---------------------------------------------------------
Title: Coordinated Ultraviolet, Optical and Radio Observations of
    RS CVn and Flare Stars
Authors: Byrne, P. B.; Butler, C. J.; Andrews, A. D.; Rodono, M.;
   Catalano, S.; Pazzani, V.; Linsky, J. L.; Bornman, P.; Haisch, B. M.
1983IBVS.2258....1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: X-ray observations of stellar flares
Authors: Haisch, B. M.
1983ASSL..102..255H    Altcode: 1983ards.proc..255H; 1983IAUCo..71..255H
  The history of stellar X-ray flare observations prior to the Einstein
  Observatory is reviewed. X-ray light curves as measured by the IPC
  are then presented for all time resolved flare events discovered as
  of July 1982 in the Einstein data set. These light curves are analyzed
  in terms of solar-like loop models to derive densities, temperatures,
  loop lengths, magnetic field strength lower limits, etc. The failure
  of the model to adequately represent the observations in the case
  of the YZ CMi flares is discussed. The relationship of X-ray to
  optical emission, and X-ray to UV emission, is considered from both
  an observational and a theoretical viewpoint. It is concluded that
  the characterization of a flare by a single, time-averaged ratio,
  L(x)/L(opt), is not physically significant.

---------------------------------------------------------
Title: Identification of Active Regions on the Eclipsing Binary
    Flare Star Pair YY Gem
Authors: Haisch, B. M.
1983iue..prop.1449H    Altcode:
  The eclipsing spectroscopic binary TY Cam is unique sand extremely
  interesting because both stars are identical dMle flare-active
  stars in a circular, short period (19.6 hr) orbit. Both stars are
  synchronously rotating; extended starspot regions, plage regions and
  regions of flare activity have previously been identified and napped
  out. Both stars are bright X-ray and 6 cm radio sources. We propose
  to Investigate the geometrical distribution of active regions on the
  stellar surfaces by taking a series of long and short wavelength IUE
  low dispersion spectra covering about 50% of just over three orbital
  periods; we will especially concentrate on taking spectra during
  tines of eclipse. In addition, the chromospheric and transition
  region fluxes will be compared to other dM and dMe stars to further
  toot the rotation-activity connection. Differential emission measure
  analysis will be used to compare active region properties to solar
  plage emission and to loop models. Intercomparisons will be made to
  photospheric variability (from simultaneous ground-based photometry
  and spectrophotometry) and to coronal variability (from simultaneous
  VLA observations of 6 cm gyroresonance emission).

---------------------------------------------------------
Title: Further observational evidence for a coronal boundary line
    in the cool star region of the H-R diagram.
Authors: Haisch, B. M.; Simon, T.
1982ApJ...263..252H    Altcode:
  Soft X-ray emission was detected from Gamma Hya and 37 Com, at
  levels of 6-8 x 10 to the -13th ergs/sq cm per sec, during 0.2-4.0
  keV observations of eight G-K giant stars obtained with the Einstein
  Observatory's Imaging Proportional Counter. Upper limits of about 3
  x 10 to the 13th ergs/sq cm per sec were determined for the remaining
  stars. These results are judged to strengthen the Ayres et al (1981)
  findings that stellar coronae whose temperature is greater than one
  million K are either very weak or entirely absent among red giants and
  supergiants, while a large range in coronal emission exists among the
  yellow giant and supergiant stars.

---------------------------------------------------------
Title: Implications of Solar Flare Observations on Stellar X-Ray
    Flares
Authors: Antiochos, S. K.; Haisch, B. M.; Stern, R. A.
1982BAAS...14..864A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Simultaneous X-ray, ultraviolet, optical, and radio
    observations of the flare star Proxima Centauri
Authors: Haisch, B. M.; Slee, O. B.; Siegman, B. C.; Nikoloff, I.;
   Candy, M.; Harwood, D.; Verveer, A.; Quinn, P. J.; Wilson, I.; Linsky,
   J. L.
1981ApJ...245.1009H    Altcode:
  Results of coordinated program of observations in the X-ray, UV,
  optical and radio regions of the dM5e flare star Proxima Centauri
  are presented. Simultaneous observations of the star were obtained
  on March 6 and March 7, 1979, by the Einstein Observatory IPC, the
  IUE SWP and LWR cameras at low dispersion, three ground-based optical
  telescopes in Australia and the Parkes 64-m radio telescope. A total
  of 10 radio bursts and six optical flares was detected during three
  nights of simultaneous radio and optical observations, which appear
  to be broadly correlated. A major X-ray flare event was detected with
  temperatures of 1.7 x 10 to the 7th and 1.2 x 10 to the 7th K during
  the rise and decay phases, respectively, respective X-ray fluxes of
  3.0 x 10 to the -11th and 3.7 x 10 to the -11th ergs/sq cm per sec,
  and changes in spectral flux distribution. No radio, optical or UV flare
  emission corresponding to the X-ray flare was detected. The X-ray flare
  is interpreted in terms of an arch model with cooling predominantly by
  X-ray radiation, with an electron density of 1.0 x 10 to the 11th/cu
  cm during the decay phase and a total arch length comparable to the
  size of the star itself. The X-ray flare observed is thus more similar
  to a typical strong solar flare than heretofore seen on a flare star.

---------------------------------------------------------
Title: Results from an extensive Einstein stellar survey.
Authors: Vaiana, G. S.; Cassinelli, J. P.; Fabbiano, G.; Giacconi,
   R.; Golub, L.; Gorenstein, P.; Haisch, B. M.; Harnden, F. R., Jr.;
   Johnson, H. M.; Linsky, J. L.; Maxson, C. W.; Mewe, R.; Rosner, R.;
   Seward, F.; Topka, K.; Zwaan, C.
1981ApJ...245..163V    Altcode:
  The preliminary results of the Einstein Observatory stellar X-ray survey
  are presented. To date, 143 soft X-ray sources have been identified with
  stellar counterparts, leaving no doubt that stars in general constitute
  a pervasive class of low-luminosity galactic X-ray sources. Stars along
  the entire main sequence, of all luminosity classes, pre-main sequence
  stars as well as very evolved stars have been detected. Early type
  OB stars have X-ray luminosities in the range 10 to the 31st to 10 to
  the 34th ergs/s; late type stars show a somewhat lower range of X-ray
  emission levels, from 10 to the 26th to 10 to the 31st ergs/s. Late type
  main-sequence stars show little dependence of X-ray emission levels upon
  stellar effective temperature; similarly, the observations suggest weak,
  if any, dependence of X-ray luminosity upon effective gravity. Instead,
  the data show a broad range of emission levels (about three orders of
  magnitude) throughout the main sequence later than F0.

---------------------------------------------------------
Title: The Status of the Corona/Wind Boundary Line in the Cool Star
    Region of the HR Diagram
Authors: Haisch, B. M.; Simon, T.
1981BAAS...13Q.784H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Corona and Chromosphere of Proxima Centauri during Flare
    and Quiescent Times
Authors: Haisch, B. M.; Linsky, J. L.; Slee, O. B.
1981BAAS...13..515H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Type Stars
Authors: Haisch, Bernard
1981iue..prop..877H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Einstein X-ray observations of Proxima Centauri and the
    surrounding region
Authors: Haisch, B. M.; Harnden, F. R., Jr.; Seward, F. D.; Vaiana,
   G. S.; Linsky, J. L.; Rosner, R.
1980ApJ...242L..99H    Altcode:
  The first detection of both quiescent and flaring soft X-ray emission
  from a dMe flare star, Proxima Centauri (dM5e) is reported. The data
  are analyzed for temporal variability and spectral characteristics. The
  quiescent state is characterized by a mean X-ray luminosity of 1.5 x 10
  to the 27th erg s/s, corresponding to a mean surface flux of 700,000
  erg s/sq cm-s, and an inferred temperature of 4-million K. The flare
  that is detected has a peak flux of 7.4 x 10 to the 27th erg s/s and
  a peak temperature of 17-million K. The implications of these data for
  models of the quiescent and flare coronae of dMe stars are discussed.

---------------------------------------------------------
Title: A practical introduction to astrometry.
Authors: Haisch, B. M.
1980JAnSc..28..205H    Altcode:
  This paper serves as a practical review of astrometry for the
  non-specialist. It presents a step-by-step guide to the origin of
  various precession, nutation and aberration terms and the application
  of those terms to astrometrical data. Detailed examples are worked
  out applying the formalism to sample calculations of mean, true and
  apparent positions. Also included is a brief discussion of the new
  (1976) set of constants which will replace the present system when the
  new fundamental astrometrical reference system, the FK5, is introduced.

---------------------------------------------------------
Title: Observations of the quiescent corona, transition region,
    and chromosphere in the dMe flare star Proxima Centauri.
Authors: Haisch, B. M.; Linsky, J. L.
1980ApJ...236L..33H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Outer atmospheres of cool stars. IV. A discussion of cool
    stellar wind models.
Authors: Haisch, B. M.; Linsky, J. L.; Basri, G. S.
1980ApJ...235..519H    Altcode:
  Possible wind models for late-type stars which appear not to have hot
  coronae and transition regions are investigated; taking Arcturus and
  the prototypical star, models with T less than approximately 20,000
  K are considered, and solutions with mass loss rates of 10 to the
  -9th solar masses per year are sought. The radiation pressure of
  L-alpha resonance scattering can exceed the force of gravity in
  the chromosphere and initiate a net outflow, but is insufficient
  to sustain a wind, except perhaps in the presence of an additional
  momentum input term such as Alfven wave pressure. It is concluded that
  L-alpha radiation-pressure-initiated winds can occur in stars to the
  right of the Linsky-Haisch dividing line in the H-R diagram between
  stars with and without transition regions and presumably hot coronae,
  and that the existence of these winds may explain energetically the
  absence of hot coronae in these stars.

---------------------------------------------------------
Title: The 2300-3000A IUE Spectrum of Alpha Orionis
Authors: Haisch, B. M.; van der Hucht, K. A.; Linsky, J. L.
1979BAAS...11..681H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: HEAO 1 observations of X-ray emission from flares in dMe stars.
Authors: Kahn, S. M.; Linsky, J. L.; Mason, K. O.; Haisch, B. M.;
   Bowyer, C. S.; White, N. E.; Pravdo, S. H.
1979ApJ...234L.107K    Altcode:
  The paper reports the detection of two X-ray flares from each of the
  nearby dMe stars, AT Mic and AD Leo, with the A-2 experiment on board
  HEAO 1. A spectrum obtained during the brighter AT Mic flare, the
  first X-ray spectrum of a stellar flare, is well matched by a thermal
  model with a temperature 3 x 10 to the 7 K and an iron K-alpha emission
  line. The X-ray luminosities derived are in the range 1.3-16 x 10 to
  the 30th ergs/s, while emission measures are in the range 1.1-14 x 10
  to the 53rd/cu cm. The estimated Lx/Lopt ratios exceed unity and are
  inconsistent with Mullan's flare model. Several scenarios to explain
  this discrepancy are proposed.

---------------------------------------------------------
Title: A comparison of emission lines in the ultraviolet spectra
    of alpha Boo (K2 IIIp), alpha Tau (K5 III), alpha Ori (M1-2 Ia-b)
    and alpha Sco (M1.5 Iab+B2.5 V).
Authors: van der Hucht, K. A.; Stencel, R. E.; Haisch, B. M.; Kondo, Y.
1979A&AS...36..377V    Altcode:
  Observations and identifications are presented of 45 emission lines in
  the near-ultraviolet spectra of Boo (K2 IIIp), x Tau (KS III), z Ori
  (M1-2 Ia-b) and 1 +2 Sco (M1.5 Iab+ B2.5 V). The useful wavelength
  ranges, A for Boo, 28( A for Tau, A for Ori and 2()()( 2400 A, 27O(
  3200 A for 1+2 Sco are covered with a resolution of 0.1 A. We have
  identified emission lines of Mg I, Fe I, Fe II, Fe III and a possible
  Si I emission line, in addition to the strong chromospheric Mg II h
  and k resonance emission lines. Several Fe I and Fe II fluorescence
  emission lines are identified, which may originate through pumping by
  the Mg II X2795 k line. Because of the lack of an intensity calibration
  only a qualitative description of the data is possible. Where possible
  we have established radial velocities for the various regions in the
  chromospheres and circumstellar envelopes of the stars. The emission
  lines of x Ori show an outflow of material from both the chromospheric
  and circumstellar regions, in contrast to a previously determined
  inflow as measured by Boesgaard and Magnan (1975). We conclude
  that we are seeing a different phase of an apparently variable mass
  motion phenomenon. We suggest an interpretation in terms of very large
  convective elements as hypothesized by Schwarzschild (1975). The other
  three stars show a blue shifted absorption component in the Mg II lines
  on top of the overall redshifted emission. The Fe III emission lines in
  the spectrum of 1 +2 Sco are due to the presence of the B star within
  the circumstellar envelope of the M star. Key words: chromosphere -
  circumstellar envelope - stars: individual - spectra: ultraviolet

---------------------------------------------------------
Title: IUE and the Search for a Lukewarm Corona
Authors: Pasachoff, J. M.; Linsky, J. L.; Haisch, B. M.; Boggess, A.
1979S&T....57..438P    Altcode:
  The use of the International Ultraviolet Explorer (IUE) to search
  for stars having neither a hot corona nor a cool outer atmosphere,
  but a lukewarm corona is outlined. An interactive computer system
  permits extensive analysis of the data immediately after transmission
  to earth, allowing the results of one exposure to influence the taking
  of subsequent exposures. The observation program is illustrated for the
  star HR 1099, noting that observations were taken while previous spectra
  were being analyzed. Observations of many stars of spectral types G and
  K lead to the construction of a border region on the Hertzsprung-Russell
  diagram between stars with hot coronas and those with cool outer
  atmospheres. Stars lying near this border region were then observed;
  however, none with lukewarm coronas was found. The interactive control
  facility in the satellite control room is considered an important
  factor in the efficient implementation of the search procedure.

---------------------------------------------------------
Title: Outer atmospheres of cool stars. I. The sharp division into
    solar-type and non-solar-type stars.
Authors: Linsky, J. L.; Haisch, B. M.
1979ApJ...229L..27L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Simultaneous X-ray, UV, Optical, and Radio Observations of
    the Flare Star Proxima Centauri
Authors: Haisch, B. M.; Linsky, J. L.; Slee, O. B.; Worden, S. P.
1979BAAS...11..471H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Radiative transfer in spherical dust shells using a generalized
    two-stream Eddington approximation.
Authors: Haisch, B. M.
1979A&A....72..161H    Altcode:
  Application of a generalized two-stream Eddington approximation to
  the problem of radiative transfer in extended, spherically symmetric
  dust shells is presented. It is assumed that the radiation field can
  be characterized by the mean intensity, the flux, and a positionally
  dependent direction cosine specifying the division into two solid-angle
  ranges. The direction cosine is not specified a priori and is a
  function of the geometry, opacity, and emissivity in the dust shell. A
  multiple-grain-size multiple-temperature-distribution dust shell is
  postulated in which isotropic and anisotropic scattering as well as
  absorption and thermal reemission are allowed. A program has been
  developed that solves for the multiple temperature distributions by
  applying the constraint of radiative equilibrium to each grain size,
  and then calculates emergent fluxes. Results of one such calculation
  are presented for a model dust shell having a maximum optical depth
  (approximately 41) in the visible, clearly showing large optical
  extinction and a moderate infrared excess.

---------------------------------------------------------
Title: Lyman alpha initiated winds in late-type stars
Authors: Haisch, B. M.; Linsky, J. L.; van der Hucht, K. A.
1979IUE1.symp..383H    Altcode: 1979STIN...8016008H
  One of the first major results of the IUE survey of late-type stars
  was the discovery of a sharp division in the HR diagram between stars
  with solar type spectra (chromosphere and transition region lines) and
  those with non-solar type spectra (only chromosphere lines). This result
  is especially interesting in view of observational evidence for mass
  loss from G and K giants and super-giants discussed recently by both
  Reimers and Stencel. In the present paper models of both hot coronae
  and cool wind flows are calculated using stellar model chromospheres as
  starting points for stellar wind calculations in order to investigate
  the possibility of having a 'supersonic transition locus' in the HR
  diagram dividing hot coronae from cool winds. It is concluded from
  these models that the Lyman-alpha flux may play an important role
  in determining the location of a stellar wind critical point. The
  interaction of Lyman-alpha radiation pressure with Alfven waves in
  producing strong, low temperature stellar winds in the star Arcturus
  is investigated.

---------------------------------------------------------
Title: A coordinated X-ray, optical, and microwave study of the
    flare star Proxima Centauri.
Authors: Haisch, B. M.; Linsky, J. L.; Slee, O. B.; Hearn, D. R.;
   Walker, A. R.; Rydgren, A. E.; Nicolson, G. D.
1978ApJ...225L..35H    Altcode:
  Results are reported for a three-day coordinated observing program
  to monitor the flare star Proxima Centauri in the X-ray, optical, and
  radio spectrum. During this interval 30 optical flares and 12 possible
  radio bursts were observed. The SAS 3 X-ray satellite made no X-ray
  detections. An upper limit of 0.08 on the X-ray/optical luminosity ratio
  is derived for the brightest optical flare. The most sensitive of the
  radio telescopes failed to detect 6-cm emission during one major and
  three minor optical flares, and on this basis an upper limit on the
  flare radio emission (1 hundred-thousandth of the optimal luminosity)
  is derived.

---------------------------------------------------------
Title: Outer Atmospheres of Cool Stars: The Sharp Division into
    Solar-Type and Alpha Orionis-Type Stars
Authors: Linsky, J. L.; Haisch, B. M.
1978BAAS...10..647L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: IUE and BUSS Observations of Alpha Orionis
Authors: Haisch, B. M.; Linsky, J. L.; van der Hucht, K. A.
1978BAAS...10..646H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Analysis of the chromospheric spectrum of O I in Arcturus.
Authors: Haisch, B. M.; Linsky, J. L.; Weinstein, A.; Shine, R. A.
1977ApJ...214..785H    Altcode:
  The ultraviolet and near-infrared spectra of O I in Arcturus are
  analyzed by a 15-level 14-transition model for O I and the Ayres-Linsky
  (1975) model chromosphere. It is found that the anomalously bright O
  I resonance lines at 1302, 1305, and 1306 A can be readily explained
  by a Ly-beta-pumped fluorescence mechanism as originally proposed by
  Bowen (1974). Observed equivalent widths of the near-infrared triplet
  and singlet lines are also consistent with the model predictions,
  but the intercombination lines at 1355 and 1359 A and near-infrared
  quintet lines may pose a problem.

---------------------------------------------------------
Title: Extreme-ultraviolet observations of flare on Proxima Centauri
    and implications concerning flare-star scaling theory.
Authors: Haisch, B. M.; Linsky, J. L.; Lampton, M.; Paresce, F.;
   Margon, B.; Stern, R.
1977ApJ...213L.119H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Extreme Ultraviolet Observations of a Flare on Proxima Centauri
    and Implications Concerning Flare Star Scaling Theory.
Authors: Haisch, B. M.; Linsky, J. L.; Bowyer, S.
1976BAAS....8..545H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Theoretical wavelength dependence of polarization in early-type
    stars.
Authors: Haisch, B. M.; Cassinelli, J. P.
1976ApJ...208..253H    Altcode:
  The wavelength dependence of linear polarization produced by
  electron scattering and modified by an absorptive opacity in the
  extended, distorted atmospheres of early-type stars is examined
  theoretically. When we use an iterative scheme, the equation of
  radiative transfer for plane polarized light is solved numerically
  for four model atmospheres representing a Wolf-Rayet star and three
  types of Be star. The extended, but heretofore spherically symmetric,
  atmosphere models are now assumed to have the shapes of either a
  rigidly rotating star (called a Roche model) or a truncated disk. The
  asymmetry provides polarization in the net observable flux. The amount
  of this polarization and its wavelength dependence are investigated
  and compared to observations. It is found that only a highly flattened
  disk can provide polarization in excess of 1 percent as is sometimes
  observed. The wavelength dependence of the models agrees with the
  observed shape of the polarization curve between the Paschen and Balmer
  edges, but does not predict an increase in polarization longward of
  the Paschen continuum nor as sharp a decrease shortward of the Balmer
  continuum as is observed.

---------------------------------------------------------
Title: Properties of the chromosphere-corona transition region
    in Capella.
Authors: Haisch, B. M.; Linsky, J. L.
1976ApJ...205L..39H    Altcode:
  Analysis of recent ultraviolet observations of the Capella binary system
  (Alpha Aur) indicates a dense geometrically narrow chromosphere-corona
  transition region in the Capella system primary (G5 III) similar in
  many respects to a solar active region. An examination of the coronal
  energy balance, together with the coronal base pressure derived from
  the line fluxes, predicts a corona with a mean temperature of 1.2
  million K and a large stellar wind consistent with observations.

---------------------------------------------------------
Title: A tensor formulation of the equation of transfer for
    spherically symmetric flows.
Authors: Haisch, B. M.
1976ApJ...205..520H    Altcode:
  A tensor formulation of the equation of radiative transfer is derived
  in a seven-dimensional Riemannian space such that the resulting
  equation constitutes a divergence in any coordinate system. After being
  transformed to a spherically symmetric comoving coordinate system, the
  transfer equation contains partial derivatives in angle and frequency,
  as well as optical depth due to the effects of aberration and the
  Doppler shift. However, by virtue of the divergence form of this
  equation, the divergence theorem may be applied to yield a numerical
  differencing scheme which is expected to be stable and to conserve
  luminosity. It is shown that the equation of transfer derived by this
  method in a Lagrangian coordinate system may be reduced to that given
  by Castor (1972), although it is, of course, desirable to leave the
  equation in divergence form.

---------------------------------------------------------
Title: An Analysis of the Chromospheric O I Lines in Arcturus
Authors: Haisch, B. M.; Linsky, J. L.; Weinstein, A.; Shine, R.
1976BAAS....8..303H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Theoretical Wavelength Dependence of Polarization in Early-Type
    Stars
Authors: Haisch, B. M.; Cassinelli, J. P.
1976IAUS...70..375H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Polarization Models for Early-Type Stars
Authors: Haisch, B. M.; Cassinelli, J. P.
1975BAAS....7..559H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Tensor Formulation of the Equation of Transfer I. Application
    to Plane Parallel Flows.
Authors: Haisch, B. M.
1975BAAS....7..449H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Polarization by rotationally distorted electron scattering
    atmospheres.
Authors: Cassinelli, J. P.; Haisch, B. M.
1974ApJ...188..101C    Altcode:
  The polarization to be expected from rotationally distorted early-type
  stars is determined using results of calculations of the transfer of
  linearly polarized light in extended atmospheres. Polarization as high
  as about 6 percent is found for a disk envelope model and 2 percent
  for a Roche atmospheric model. The factors controlling the direction of
  the polarization are discussed. Plausible explanations are offered for
  the anomalous wavelength dependence of both the degree of polarization
  in the Wolf-Rayet star HD 50896 and of the direction of polarization
  in the Be star HD 45677. Subject headings: atmospheres, stellar -
  Be stars - polarization - radiative transfer - Wolf-Rayet stars

---------------------------------------------------------
Title: Maximum Net Polarization for Rotationally Distorted Electron
    Scattering Atmospheres.
Authors: Cassinelli, J. P.; Haisch, B. M.
1973BAAS....5..337C    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Photometric observations of the star cluster NGC 2141.
Authors: Burkhead, M. S.; Burgess, R. D.; Haisch, B. M.
1972AJ.....77..661B    Altcode:
  No abstract at ADS