explanation blue bibcodes open ADS page with paths to full text
Author name code: muench
ADS astronomy entries on 2022-09-14
author:"Munch, Guido"
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Title: Capturing Software Citations in Astronomy and Planetary
Sciences
Authors: Henneken, E. A.; Muench, G.; Holm Nielsen, L.;
Blanco-Cuaresma, S.; Accomazzi, A.
2019LPI....50.1569H Altcode:
This poster discusses the importance of capturing software citations
and how this has been implemented in the Asclepias project of the AAS,
ADS, and Zenodo.
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Title: Turbulence in the Interstellar Medium: a Retrospective Review
Authors: Münch, Guido
1999intu.conf....1M Altcode:
No abstract at ADS
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Title: The Universe at Large
Authors: Münch, Guido; Mampaso, Antonio; Sánchez, Francisco
1997unla.book.....M Altcode:
The Universe at Large presents a unique survey of key questions
outstanding in contemporary astronomy and cosmology. In this
timely volume, eleven of the world's greatest living astronomers and
cosmologists present personal views of what problems must be addressed
by future research. Allan Sandage presents a 23-point plan to reach
a full understanding of the large-scale structure in the Universe;
Geoffrey Burbidge looks at the future of the Quasi Steady State
alternative to the Big Bang; E. Margaret Burbidge, Donald Osterbrock
and Malcolm Longair discuss active galactic nuclei (AGN); Igor Novikov,
Donald Lynden-Bell, Martin Rees and Rashid Sunyaev look at the physics
of black holes; and Bernard Pagel and Hubert Reeves concentrate on
what we don't yet understand about elements in the cosmos. This book
provides a unique review of our current understanding in astronomy
and cosmology and a host of profitable research ideas for graduate
students and researchers.
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Title: The Universe at Large
Authors: Münch, Guido; Mampaso, Antonio; Sánchez, Francisco
1997ual..book.....M Altcode:
Preface; 1. Astronomical problems for the next three decades
Allan Sandage; 2. New vistas in cosmology and cosmogony Geoffrey
Burbidge; 3. Omega, dark mass and galactic history Donald Lynden-Bell;
4. Observations of QSOs which are critical for cosmology E. Margaret
Burbidge; 5. Nature, structure, refuelling and evolution of AGNs
Donald Osterbrock; 6. The high energy radiation of active galactic
nuclei Malcolm S. Longair; 7. Physics and astrophysics of black holes
Igor Novikov; 8. Galaxy formation and quasars - progress and prospects
Martin J. Rees; 9. Cosmic abundances Bernard E. J. Pagel; 10. Clues
to early development of galaxies Hubert Reeves; 11. The observational
appearance of accreting black holes in X-ray binaries Rashid Sunyaev;
12. Reflections on the key problems Malcolm S. Longair; Index.
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Title: The Universe at large. Key issues in astronomy and cosmology.
Authors: Münch, G.; Mampaso, A.; Sánchez, F.
1997ualk.book.....M Altcode:
This book provides a unique review of our current understanding in
astronomy and cosmology, and a host of ideas for profitable future
research.
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Title: Obituary: Jerome Kristian, 1934-1996
Authors: Munch, Guido
1997BAAS...29.1476M Altcode:
No abstract at ADS
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Title: The Universe at Large, Key Issues in Astronomy and Cosmology
Authors: Munch, Guido; Mampaso, Antonio; Sánchez, Francisco
1997ulki.book.....M Altcode:
The Universe at Large presents a unique survey of key questions
outstanding in contemporary astronomy and cosmology. In this
timely volume, eleven of the world's greatest living astronomers
and cosmologists present their personal views of what problems must
be addressed by future research. Allan Sandage presents a 23-point
plan to reach a full understanding of the largescale structure in
the Universe; Geoffrey Burbidge looks at the future of the Quasi
Steady State alternative to the Big Bang; active galactic nuclei
(AGN) are discussed by E. Margaret Burbidge, Donald Osterbrock and
Malcolm Longair; Igor Novikov, Donald Lynden-Bell, Martin Rees and
Rashid Sunyaev look at the physics of black holes; and Bernard Pagel
and Hubert Reeves concentrate on what we don't yet understand about
elements in the cosmos. This book provides a unique review of our
current understanding in astronomy and cosmology, and a host of ideas
for profitable future research - for graduate students and researchers.
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Title: Complex interstellar absorption lines of C_2_ in the Cygnus
OB association
Authors: Gredel, R.; Muench, G.
1994A&A...285..640G Altcode:
Measurements of interstellar absorption lines in the (1,0) band of
the C_2_ Phillips system, around 1.015 μm, are reported for the
stars Nos. 12 and 5 of the Cyg OB2 association. The R(0), Q(2), and
Q(4) lines, at a resolving power of 65,000, show a complex structure,
with four discrete components in No. 12 and three in No. 5. The radial
velocities of the various components, spread over a range of 22 km/s ,
agree in both stars, suggesting their origin in similar spatio-kinematic
structures. The relative intensities between the various components are
not the same in the two stars, but the net C_2_ column densities derived
for the two stars result nearly proportional to their respective B-V
color excesses, as it has been found in stars of smaller reddening. A
typical clump of absorbing gas, in the close neighborhood or within
the association, has been characterized by an upper limit of 5 pc in
linear dimensions and a mass of 200 M<SUB>sun</SUB>_. The low emission
of the association in the free-free radio continuum is suggested to
be a result of the removal of HII-gas by the powerful winds known to
be emitted by its members.
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Title: Detection of Hα Emission on High Velocity 21-CENTIMETER Clouds
Authors: Muench, Guido; Pitz, Eckhart
1990IAUS..139..193M Altcode:
The measurement of H-alpha emission on two high galactic latitude clouds
known to emit 21 cm lines with local standard of rest velocities of -50
and -85 km/s is reported. The H-alpha lines have been found nearly at
the velocities of the 21 cm features and have emission rates of 0.2
Rayleigh. The diffuse Lyman continuum intensity required to produce
H I ionization at the measured rate is in agreement with the direct
measurements made with the ultraviolet spectrometer of the Voyager
2 spacecraft.
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Title: Highly excited molecular hydrogen in M 42 and other nebulae.
Authors: Hippelein, H. H.; Muench, G.
1989A&A...213..323H Altcode:
Measurements of the S(5), S(7), S(10), and S(11) quadrupole lines of
the (2,0) band of H2 in the Orion Nebula (M 42) are presented. These
measurements showed the following features: (1) the radial velocity
characteristics consistent with those of microwave lines emitted by the
Orion Molecular Cloud (OMC); (2) an intrinsic line width of 4.7 km/sec,
exceeding that measured in microwave lines; (3) a surface brightness
distribution in S(11) with a nearly circular symmetry around and a
maximum at the Trapezium; (4) and a net column density of vibrationally
excited H2 that can be accounted for by fluorescent excitation models
with parameters appropriate for the OMC. A rotational temperature of
about 11,000 K was observed, in excess of that predicted by radiative
excitation.
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Title: H<SUB>α</SUB>-emission in directions toward high velocity
21cm clouds
Authors: Münch, Guido; Pitz, Eckhart
1989LNP...350..373M Altcode: 1989IAUCo.120..373M; 1989sdim.conf..373M
Measurements of H<SUB>α</SUB>-emission in fields known to emit 21cm
radiation at intermediate and high velocities are presented. The
observations are partial results of a survey being carried out at
the Calar Alto Observatory with a dedicated Fabry-Perot spectrometer
of 15cm aperture, providing velocity and angular resolutions of 11km
s<SUP>-1</SUP> and 0.5 deg<SUP>2</SUP>. The limited material available
indicates that the H<SUB>α</SUB>-emission, when detected at a radial
velocity nearly the same as that measured in 21cm, appears more extended
in the sky than the HI-radiation.
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Title: Highly excited molecular hydrogen in orion
Authors: Hippelein, Hans H.; Münch, Guido
1989LNP...350..323H Altcode: 1989IAUCo.120..323H; 1989sdim.conf..323H
No abstract at ADS
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Title: Rotational structure of the (2, 0) Phillips band of C2 in
Comet P/Halley
Authors: Appenzeller, I.; Muench, G.
1987A&A...187..465A Altcode:
The results of the study of a digital echellogram of the nuclear region
of comet Halley, containing the (2,0) Phillips band of C<SUB>2</SUB>
fully resolved, are presented. The intensities of individual lines,
measured from the R-branch head up to R36, Q30, and P24, indicate a very
high degree of rotational excitation. The population of the levels from
where the lines arise, when approximated by a Boltzmann distribution,
is found to be characterized by a temperature higher than that obtained
from the Swan bands in other comets. An absolute calibration of the
line fluxes has been obtained from narrow band CCD-imagery, to make
feasible their comparison with measurements in the Swan system,
probably carried out by other observers of comet Halley.
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Title: Photometry of comet P/Halley at near post-perihelion phases
Authors: Neckel, T.; Muench, G.
1987A&A...187..581N Altcode:
Photometric measurements of Halley's comet at phases around its recent
perigee are presented. Narrow band filters isolating the C<SUB>2</SUB>
Swan band emission and a neighboring continuum, besides the standard
UBV, have been used with 4 nucleus centered field stops subtending
angles between 41arcsec and 1050arcsec. The brightness fluctuations
detected, especially conspicuous in C<SUB>2</SUB> and the nearby
continuum, indicate a period of 7.3 days. Some evidence for the double
peaked nature of the periodic variation is marginally present.
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Title: Geschwindigkeits-Schnitte von Planetarischen Nebeln
Authors: Hippelein, H.; Münch, G.
1987MitAG..68..258H Altcode:
No abstract at ADS
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Title: GIOTTO Flights Dynamics Report No. 1 part 4
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
1986gfd..rept....4M Altcode:
Details of the Orbit determination of Comet Halley during the GIOTTO
Flyby in March 1986 are discussed
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Title: Periodic Comet Halley (1982i)
Authors: Munch, G.; Hippelein, H.; Hessmann, F.; Gredel, R.; Celnik,
W. E.; Schulz, R.; Weissbauer, K.; West, R. M.; Pedersen, H.; Gelly,
B.; Le Bertre, T.; Sheffer, Y.; Fleet, R.; Bennett, J. C.; Campos, J.
1986IAUC.4183....1M Altcode:
G. Munch, H. Hippelein, F. Hessmann and R. Gredel, Max-Planck- Institut
fur Astronomie, report measurements of [C I] 985-nm emission with
the 1.2-m telescope of the Calar Alto Observatory and a 2-etalon
spectrometer at 0.04-nm resolution in field integrated mode. On
1985 Dec. 14, through a 2' stop centered on the nucleus, an emission
rate of E = 8 +/- 1 Ray and a radial velocity within 1 km/s of the
ephemeris value (IHW orbit No. 22) were found. At 4' tailward from
the nucleus E ~ 2 Ray, only 5 percent of that in airglow OH(3,0)P2(2)
at 984.848 nm. The corresponding metastable production rate along
the sampled nucleus centered column is Q = 10**26.7/s. Essentially
the same results were found on Dec. 22. W. E. Celnik, R. Schulz and
K. Weissbauer, European Southern Observatory, report tail lengths on
Feb. 20.4 UT of 59' (red), 20' (blue), 40' (CO+) and 33' (CN), and an
intense antitail in p.a. 90. On Feb. 21.4 the tail lengths were 2.5 deg
(red), 4.3 deg (blue), 2.6 deg (CO+) and 0.75 deg (CN). On Feb. 22.4
there were ion tails in p.a. 106 and 92, and dust tails in p.a. 65,
50, 34, 358 and 322; maximum tail lengths were 4.1 deg (red, blue),
1.8 deg (CO+) and 0.57 deg (CN). On Feb. 24.4 the CO+ tail length was
9.2 deg; a bright CO+ core of diameter 15" was embedded in a faint,
diffuse coma 9'2 in diameter; in red light concentric bow shocks were
detected at distances 14", 60" and 140" from the core. CCD observations
by R. M. West, H. Pedersen and B. Gelly on Feb. 23 showed the tail
structure reported on IAUC 4179 changed as follows: 1, broad, diffuse
to 75' in p.a. 270, strong kink at 225, maximum length 240', additional
sharp loop to south 45' in 260; 2, stong, diffuse, to 130' in 277;
3, diffuse to 100' in 286; 4, diffuse to 135' in 317; 5, diffuse,
stubby, to 100' in 333; 6, strong, narrow to 95' in 0 at west edge
of broad, diffuse, with other extreme 55' in 30; 7, sharp edge to 25'
in 67. T. le Bertre reports that infrared photometry shows variations
of up to 1.5 mag from day to day; representative are the data in L
(diaphragm 30", uncertainty generally 0.05 mag): Feb. 16.4 UT, -0.19;
17.4, +0.74; 18.4, -0.73; 19.4, +0.16; 20.4, -0.54; 22.4, +0.37;
23.4, +0.04. Total visual magnitude estimates: Feb. 21.51 UT, 3.0
(Y. Sheffer, Austin, TX, 7 x 50 binoculars); 22.13, 3.9 (R. Fleet,
Harare, Zimbabwe, 11 x 80 binoculars); 23.11, 3.5 (Fleet); 24.10, 3.0
(J. C. Bennett, Pretoria, South Africa, 0.13-m refractor); 25.11, 3.0
(J. Campos, Durban, South Africa, 0.13-m refractor).
---------------------------------------------------------
Title: Interstellar molecular carbon in distant supergiants.
Authors: Gredel, R.; Muench, G.
1986A&A...154..336G Altcode:
The results of a search for interstellar C<SUB>2</SUB> lines in
the spectrum of southern reddened supergiants are reported. The
C<SUB>2</SUB> excitation parameters along the lines of sight to
HD 169454 and BD -14°5037, both in the Sct OB3 association, have
been determined. Radiative excitation effects of high rotational
levels were found in HD 169454. The C<SUB>2</SUB> lines in BD
-14°5037 are clearly double. A spectrum of HD 92693, in Car OB1,
shows C<SUB>2</SUB> lines weak in proportion to its color excess
E<SUB>B-V</SUB>, but otherwise the column densities N(C<SUB>2</SUB>)
for all stars so far observed appear linearly correlated to
E<SUB>B-V</SUB>. Through the known relation of E<SUB>B-V</SUB> with
molecular hydrogen column density N(H<SUB>2</SUB>), a mean columnar
abundance N(C<SUB>2</SUB>)/N(H<SUB>2</SUB>) = 3.0×10<SUP>-8</SUP>
has been estimated, which agrees with theoretical predictions for the
C<SUB>2</SUB> abundance in dense molecular clouds.
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Title: GIOTTO Flights Dynamics Report No. 1 part 3
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
1986gfd..rept....3M Altcode:
Details of the Orbit determination of Comet Halley for the GIOTTO
Flyby in March 1986 are discussed
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Title: Die Linien der 2-0 Vibrationsbande des molekularen Wasserstoffs
im Orion-Nebel
Authors: Hippelein, H. H.; Münch, G.
1986MitAG..67..358H Altcode:
No abstract at ADS
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Title: Internal Dust in H II Regions
Authors: Münch, G.
1985MitAG..63...65M Altcode:
A review is given of the observable effects that scattering dust
internal to H II-regions may have on their characteristic visual
spectrum. The intrinsic color of optically thin lines is discussed, with
special reference to the Balmer decrement. The effects of scattering
on the transmission of line radiation formed in the deep interior of
H II-regions is considered. Recent observations of He I λλ10829-30
emission line profiles in M42 are discussed, together with their
interpretation through radiative transfer calculations. Absorption
line observations of He I λλ10829-30 on θ<SUP>1</SUP>Ori C and
θ<SUP>2</SUP>Ori A are presented and discussed in relation to the
corresponding emission lines.
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Title: Internal reddening of H II-regions and HH-objects, with
special reference to NGC 896(W3).
Authors: Gomez Garrido, P.; Muench, G.
1984A&A...139...30G Altcode:
The effect of scattering by dust internal to H II regions on their
spectral characteristics has been studied on the basis of simple
analytical models, for assumed universal optical parameters of the
dust. A procedure to determine the external interstellar extinction
and the internal gas to dust abundance ratio of H II regions has been
developed and applied as a test to the Orion Nebula. Newly acquired
observations of the H II region NGC 896 have been analyzed to identify
the effects of internal dust on its spectrum and to establish its
relationship to the background radio source W3 (cont.). Finally, the
effects that the probable existence of scattering dust internal to
HH-objects might have on the color of their spectrum has been included.
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Title: GIOTTO Flights Dynamics Report No. 1 part 2
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
1984gfd..rept....2M Altcode:
Details of the observation strategy and Orbit determination of Comet
Halley for the GIOTTO Flyby in March 1986 are discussed
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Title: Detection of H2 emission at 1.064 MU M in the Orion Nebula.
Authors: Muench, G.; Hippelein, H.; Pitz, E.
1984A&A...135L..11M Altcode:
Emission of H<SUB>2</SUB> in the S7 line of the (2,0) band at 1.064
μm, from regions of M42 emitting H<SUB>2</SUB> lines in the IR, is
reported. The line profile is asymmetric, with an extended violet
wing, similar to that of (1,0)S1 at 2.1 μm. Regions not emitting
(1,0)S1 show a sharp symmetric line centered at the wavelength
expected for H<SUB>2</SUB>(2,0)S7, which is, nevertheless, considered
as unidentified. The extinction optical depth at (1,0)S1, derived from
a comparison of its violet shifted flux with that at S7, is nearly in
agreement with the value obtained from IR data, when the scattering
of S7 radiation by internebular dust is taken into account. It is
estimated that over 60% of the measured (2,0)S7 emission has undergone
scattering in its transport through the nebula.
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Title: GIOTTO Flights Dynamics Report No. 1 part 1
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
1984gfd..rept....1M Altcode:
Details of the Orbit determination of Comet Halley for the GIOTTO
Flyby in March 1986 are discussed
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Title: The Effects of Scattering by Internal Dust on the Spectra of
Emission Nebulae
Authors: Munch, G.
1983RMxAA...7..229M Altcode:
No abstract at ADS
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Title: NGC 2359 : the HII-region driven by the WR-star HD 56925.
Authors: Goudis, C.; Hippelein, H.; Muench, G.
1983A&A...117..127G Altcode:
The results of a kinematic study of NGC 2359, from 21 interferometric
profiles of [O III] λ5007 and [N II] λ6583, are presented. All
profiles share a component at V<SUB>LSR</SUB>=54 km s<SUP>-1</SUP>,
identified with the systemic velocity. Over the central core, [O III]
shows components at ±30 km s<SUP>-1</SUP> from the centroid, not
seen in [N II]. The relative intensities of the displaced components
indicates their origin in tenuous gas seen pervading bright filaments,
which move nearly with the systemic velocity. It is proposed that the
tenuous gas is an expanding shell driven by the stellar wind from the
exciting WR-star, while the filaments are post-shock manifestations of
density fluctuations in the external medium overrun by the shell. The
problems offered by the joint interpretation of optical and microwave
CO line data are reconsidered and possible avenues to their solution
are suggested.
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Title: Der Cassegrain-Doppelspektrograph für das 3.5m-Teleskop
Authors: Solf, J.; Münch, G.
1983MitAG..60..473S Altcode:
No abstract at ADS
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Title: Physik-Nobelpreis 1983 für W. A. Fowler und S. Chandrasekhar.
Authors: Münch, G.
1983S&W....22R.572M Altcode:
No abstract at ADS
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Title: Physik-Nobelpreis 1983 für S. Chandrasekhar und W. A. Fowler.
Authors: Münch, G.
1983S&W....22Q.572M Altcode:
No abstract at ADS
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Title: Observations of forbidden C I emission in Orion A (M42)
and Orion B (NGC 2024)
Authors: Munch, G.; Hippelein, H.
1982NYASA.395..170M Altcode:
A map of Orion A in radiation of forbidden C I wavelength 9850, with
a resolution of 80 arcsec, down to a level of intensity 20 Ray, is
obtained. The brightness distribution in forbidden C I is found to
be flatter than that in H-alpha, with the apparent intensity ratio
forbidden C I/H-alpha varying between 0.006-0.0004. A similar map of
Orion B, with a resolution of 2 arcmin, down to a level of 7 Ray, is
found to demonstrate that the visually conspicuous central obscuration
lane, behind which the maximum continuum radio emission arises, appears
to be bright in forbidden C I. A high-resolution profile of forbidden
C I wavelength 9850 in Orion A indicates that its FWHM is 6.1 km/s,
significantly smaller than that of any other nonradio nebular line. It
is concluded that the forbidden C I emission likely arises either by
recombination in cool C II regions or by being excited by shocks.
---------------------------------------------------------
Title: Max-Planck-Institut für Astronomie, D-6900
Heidelberg-Königstuhl, Federal Republic of Germany. Centro
Astronómico Hispano-Alemán, Almeria, Spain. Report for the period
1 January - 31 December 1980.
Authors: Münch, G.
1982BAAS...14..279M Altcode:
No abstract at ADS
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Title: S 106 - an H II-region driven by a stellar wind
Authors: Hippelein, H.; Muench, G.
1981A&A....99..248H Altcode:
High resolution interferometric observations of the forbidden S
III 9531 A line emitted by the peculiar emission nebula S 106 are
presented. Observations were carried out with a Fabry-Perot scanner
attached to the 1.2 m telescope of the Calar Alto Observatory in
June and October 1979. Obtained profiles are broad, some covering a
radial velocity range exceeding 100 km/s, and asymmetric around their
peak intensity. Profiles in the north emission lobe show an excess
of positive over negative velocity, while those in the south lobe
exhibit the reverse asymmetry; velocity centroids define a kinematic
distance between 0.5 and 1.0 kpc. Measured line intensities and 6-cm
flux densities show the line formation path length to be 1/100 of the
nebular dimensions on the plane of the sky. It is suggested that the
nebular spectrum originates in a thin layer of gas confined by stellar
wind from the exciting star to the surface of a two-lobe cavity. The
nearly symmetric appearance of the nebula is attributed to the density
distribution prevailing within the disk-like complex of interstellar
matter in which the single exciting star was formed.
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Title: Wavelengths and profiles of the (SIII) 3p2,1-1d2 lines in
some emission nebula.
Authors: Hippelein, H.; Muench, G.
1981A&A....95..100H Altcode:
High resolution profiles of the nebular (S III) forbidden lines
in the integrated light of a number of bright emission nebulae are
presented. The radial velocities of the objects, determined in the
past with slit spectrographs, have been adopted to transform apparent
wavelengths of the profiles' centroids to the laboratory system. The
strongest line 3P2-1D has been found 0.8 A bluewards from the wavelength
predicted from term values.
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Title: Scientific results from the pioneer Saturn infrared radiometer
Authors: Orton, G. S.; Ingersoll, A. P.; Froidevaux, L.; Neugebauer,
G.; Munch, G.; Chase, S. C.
1981AdSpR...1h.179O Altcode: 1981AdSpR...1..179O
The Pioneer 11 Infrared Radiometer instrument made observations of
Saturn and its rings in broadband channels centered at 20 and 45 μm
and obtained whole-disk information on Titan. A planetary average
effective temperature of 96.5+/-2.5 K implies a total emission 2.8
times the absorbed sunlight. Correlation with radio science results
implies that the molar fraction of H<SUB>2</SUB> is 90+/-3% (assuming
the rest is He). Temperatures at the 1 bar level are 137 to 140 K;
regions appearing cooler may be overlain by a cloud acting as a 124
K blackbody surface. A minimum temperature averaging 87 K is reached
near 0.06 bars. Ring boundaries and optical depths are consistent
with those at optical wavelengths. Ring temperatures are 64-86 K on
the south (illuminated) side, ~54 K on the north (unilluminated) side,
and at least 67 K in Saturn's shadow. There is evidence for a south to
north drop in ring temperatures. Titan's 45 μm brightness temperature
is 75+/-5 K.
---------------------------------------------------------
Title: Max-Planck-Institut für Astronomie, D-6900
Heidelberg-Königstuhl, Federal Republic of Germany. Centro
Astronómico Hispano-Alemán, Almeria, Spain. Report for the period
1 January - 31 December 1979.
Authors: Münch, G.
1981BAAS...13Q.226M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Max-Planck-Institut für Astronomie, D-6900
Heidelberg-Königstuhl, Federal Republic of Germany. Centro
Astronómico Hispano-Alemán, Almeria, Spain. Report for the period
1 January to 31 December 1979.
Authors: Münch, G.
1981BAAS...13R.226M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Metallarme Subdwarfs der Spektraltypen F und G
Authors: Gehren, T.; Hippelein, H.; Münch, G.
1981MitAG..52...68G Altcode:
No abstract at ADS
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Title: Scientific results from the Pioneer Saturn Infrared Radiometer.
Authors: Orton, G. S.; Ingersoll, A. P.; Froidevaux, L.; Neugebauer,
G.; Münch, G.; Chase, S. C.
1981ppe..conf..179O Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Das Fabry-Perot-Interferometer des MPI für Astronomie
Authors: Hippelein, H.; Münch, G.
1981MitAG..54..193H Altcode:
No abstract at ADS
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Title: A study of the Jovian forbidden line S II nebula at high
spectral resolution
Authors: Trauger, J. T.; Muench, G.; Roesler, F. L.
1980ApJ...236.1035T Altcode:
Observations of forbidden line S II 6716-6731 A emissions from the
Jovian magnetosphere have been carried out with a PEPSIOS spectrometer
at the Hale 5 m telescope. Spectral resolving power was sufficient to
resolve the forbidden line S II line widths. From measured 6716-6731
A doublet ratios and spectral line widths a thermal plasma is found
characterized by temperatures about 2 x 10 to the 4th K and electron
densities about 2000 cu cm. The source of forbidden line S II emissions
was centered within a toroidal region of radius 5 Jupiter radii
(inside the orbit of Io), with tight latitudinal confinement near the
equilibrium equator for ions in the tilted corotating Jovian magnetic
field, and significant long-lived longitudinal structure.
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Title: Saturn's Atmosphere and Energy Balance, Ring Temperatures,
and Detection of Titan by the Pioneer Saturn Infrared Radiometer
Authors: Ingersoll, A. P.; Orton, G. S.; Neugebauer, G.; Munch, G.;
Chase, S.
1980BAAS...12..435I Altcode:
No abstract at ADS
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Title: The effects of seeing on the reflected spectrum of Uranus
and Neptune
Authors: Munch, G.; Hippelein, H.
1980A&A....81..189M Altcode:
The results of a redetermination of the rotational periods of Uranus
and Neptune, based on spectrograms obtained with the coude spectrograph
of the 5 m Hale telescope, are presented. The effects of image motion
on the shape of the spectral lines reflected by a planet rotating as
a solid body and coherently scattering solar light, has been studied
analytically. A general relation between the seeing transformed
velocities at any point on the disk and those at the equator is
established. It is shown that, for the case of Gaussian seeing, the
brightness continuum of the smeared disk contains all the information
required to derive the shape of the reflected lines. The shift, change
in r.m.s. width, and asymmetry of the seeing transformed lines at the
equator have been numerically evaluated for the brightness distribution
of Uranus determined from Stratoscope II.
---------------------------------------------------------
Title: Pioneer Saturn Infrared Radiometer: Preliminary Results
Authors: Ingersoll, A. P.; Orton, G. S.; Munch, G.; Neugebauer, G.;
Chase, S. C.
1980Sci...207..439I Altcode:
The effective temperature of Saturn, 94.4 + 3 K, implies a total
emission greater than two times the absorbed sunlight. The infrared
data alone give an atmospheric abundance of H<SUB>2</SUB> relative to
H<SUB>2</SUB> + He of 0.85 ± 0.15. Comparison of infrared and radio
occultation data will give a more precise estimate. Temperature at the
1-bar level is 137 to 140 K, and 2.5 K differences exist between belts
and zones up to the 0.06-bar level. Ring temperatures range from 60 to
70 K on the south (illuminated) side and from < 60 to 67 K in the
planet's shadow. The average temperature of the north (unilluminated)
side is ~ 55 K. Titan's 45-micrometer brightness temperature is 80 ±
10 K.
---------------------------------------------------------
Title: Max-Planck
Authors: Munch, G.
1980BAAS...12..241M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Study of the Jovian [SII] and [SIII] Nebulae at High
Spectral Resolution.
Authors: Trauger, J. T.; Munch, G.; Roesler, F.
1979BAAS...11..591T Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar System Studies - Jupiter Imaging at 5-MICRONS - Jupiter
Magnetosphere - Infrared Observations of Planets - Diameter of Pluto
Authors: Kowal, C.; Goldreich, P.; Terrile, R. J.; Westphal, J.;
Trauger, J.; Munch, G.; Roesler, F. L.; Soifer, B. T.; Matthews, K.;
Neugebauer, G.; Sargent, W. L. W.; Boksenberg, A.; Arnold, S. J.
1979haob.rept..721K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Guest Investigators
Authors: Madore, B. F.; Mekler, Y.; Miller, H. R.; Munch, G.;
Hippelein, H. H.; Ney, E. P.; Hatfield, B. J.; Peach, J. V.; Godwin,
J. G.; Dixon, K. L.; Pesch, P.; Phillips, M. M.; Rubin, V. C.;
Burstein, D.; Shoemaker, E. M.; Helin, E. F.; Shorthill, R. W.;
Smith, D. W.; Johnson, P. E.; Simkin, S. M.; Szkody, P.; Ulrich,
R. K.; Usher, P. D.; van den Bergh, S.
1979haob.rept..788M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: High-velocity Features in M 42 Driven by Stellar Winds
Authors: Taylor, K.; Munch, G.
1978A&A....70..359T Altcode:
Summary. Interferometric Hoc and [N ii] line profiles for areas of M 42
near 62 Ori A, containing small scale cloudlets with enhanced emission,
are presented. The supersonic velocities, with respect to the nebula,
found for the cloudlets are ascribed to shocks driven by the stellar
wind emitted by 62 Ori A. The similarity solution for the equations
describing the flow of a stellar wind through a uniform H il-medium
has been generalized to allow for the presence of small scale density
inhomogeneities. The short dynamical time scale, 400 yr, determined by
the measured positions and velocities of the cloudlets, is interpreted
as a manifestation of the variability of the pressure exerted by the
shocked stellar wind. Key words: emission nebulae - stellar winds
---------------------------------------------------------
Title: Neutral carbon emission in M42.
Authors: Hippelein, H.; Muench, G.
1978A&A....68L...7H Altcode:
The detection and measurement of the forbidden C I lines at 9850
and 8727 A emitted by the Orion Nebula are reported. Typical values
for the electron density needed to excite the lines collisionally
in the H II-H I transition layers and for the neutral carbon column
density are evaluated. The carbon ionization equilibrium is accounted
for by invoking the predominance of charge exchange over radiative
processes. Implications for the topology of the transition layers
are suggested.
---------------------------------------------------------
Title: A redetermination of the Uranus rotation period.
Authors: Trauger, J. T.; Roesler, F. L.; Muench, G.
1978ApJ...219.1079T Altcode:
The rotation velocity of Uranus has been measured by a comparison
of spectroscopic profiles for the 5281.8 A Fraunhofer line reflected
from Uranus and the moon. This method yields a rotation velocity which
is insensitive to atmospheric seeing conditions. Our value for the
equatorial velocity is 3.5 + or - 0.4 km/sec.
---------------------------------------------------------
Title: High Resolution Measurement of Neutral Carbon Emission Lines
in the Orion Nebula
Authors: Hippelein, H. H.; Münch, G.
1978hrs..conf..394H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Angular Dimension of the Circumstellar Envelope of µ Cephei
Measured with a Pepsios Spectrometer
Authors: Münch, G.; Roesler, F.; Trauger, J.
1978hrs..conf..660M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: (Abstract) Does Jupiter Have a "Mini-Corona"?
Authors: Munch, G.; Roesler, F.; Trauger, J.
1977PASP...89..619M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A search for the H<SUB>2</SUB> (3,0) S1 line in the spectrum
of Titan.
Authors: Muench, G.; Trauger, J. T.; Roesler, F. L.
1977ApJ...216..963M Altcode:
Results are reported for measurements of the quadrupole S1 line of the
(3, 0) absorption band of H2 in spectra of Titan, which were performed
at an effective resolution of 0.09 A by scanning with a PEPSIOS
spectrometer over a range of 0.85 A centered at the expected position
of the investigated line and sampling in 80 contiguous channels. No
statistically significant H2 (3, 0) S1 feature is found in the spectra,
but a three-sigma upper limit of 3 mA is set for the equivalent width
of the S1 line that might be present in a co-added spectrum. It is
concluded that these measurements do not provide any evidence for the
presence of H2 in the atmosphere of Titan.
---------------------------------------------------------
Title: Study of Jupiter's Corotating SII Nebula at High Spectral
Resolution
Authors: Munch, G.; Trauger, J. T.; Roesler, F. L.
1977BAAS....9..465M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Io: morphology of its sodium emission region.
Authors: Muench, G.; Bergstralh, J. T.
1977PASP...89..232M Altcode:
Results of experiments carried out to obtain two-dimensional images of
the sodium emission region associated with Io are presented. Through
multislit spectrograms and Perot-Fabry interferograms, the dependence
of the Na-emission distribution on Jupiter's magnetic field is
demonstrated. The time scale of the observed changes in the Na emission
is shown to require electron fluxes in the Jovian magnetosphere one
order of magnitude larger than those obtained by an extrapolation of
the proton fluxes measured in situ from the Pioneer 10 spacecraft.
---------------------------------------------------------
Title: Herbig-Haro object in the Orion Nebula.
Authors: Munch, G.
1977ApJ...212L..77M Altcode:
Spectral and kinematic characteristics are reported for a double
Herbig-Haro object originally observed in forbidden O I 6300-A emission
in the Orion Nebula (M42). Spectral observations in forbidden lines
of O I and S II indicate that one component has a heliocentric radial
velocity of -240 km/s and the other component exhibits no significant
velocity shift relative to the lines of M42. Rough estimates of some
parameters of the two components are offered as evidence in favor
of the hypothesis that the spectra of all Herbig-Haro objects are
shock-excited.
---------------------------------------------------------
Title: Infrared Thermal Mapping of the Martian Surface and Atmosphere:
First Results
Authors: Kieffer, H. H.; Martin, T. Z.; Chase, S. C., Jr.; Miner,
E. D.; Palluconi, F. D.; Muench, G.; Neugebauer, G.
1976Sci...193..780K Altcode:
The Viking infrared thermal mapper measures the thermal emission of the
martian surface and atmosphere and the total reflected sunlight. With
the high resolution and dense coverage being achieved, planetwide
thermal structure is apparent at large and small scales. The thermal
behavior of the best-observed areas, the landing sites, cannot
be explained by simple homogeneous models. The data contain clear
indications for the relevance of additional factors such as detailed
surface texture and the occurrence of clouds. Areas in the polar night
have temperatures distinctly lower than the CO<SUB>2</SUB> condensation
point at the surface pressure. This observation implies that the annual
atmospheric condensation is less than previously assumed and that
either thick CO<SUB>2</SUB> clouds exist at the 20-kilometer level or
that the polar atmosphere is locally enriched by noncondensable gases.
---------------------------------------------------------
Title: Mariner 10 Infrared Radiometer Results: Temperatures and
Thermal Properties of the Surface of Mercury
Authors: Chase, S. C., Jr.; Miner, E. D.; Morrison, D.; Muench, G.;
Neugebauer, G.
1976Icar...28..565C Altcode: 1976IAUCo..34..565C
Mariner 10 infrared brightness temperatures of the surface of Mercury at
11 and 45 μm are presented. The data were obtained during the first
flyby along a nera-equatorial swath extending from 17 hours local
time through local midnight to 9 hours local time. For an assumed
emissivity of 0.9, derived surface thermal inertias are between
0.0031 and 0.0031 cal cm<SUP>-2</SUP>sec<SUP>-1/2</SUP>K<SUP>-1</SUP>
and the implied minimum predawn surface kinetic temperature for the
warm pole at longitude 270° is near 93 K. Several pronounced thermal
inhomogeneities were seen, one of which appears to coincide with a
region of high radar reflectivity. The derived thermal properties and
the electrical skin depth and loss tangent fall within the range of
values found on the Moon.
---------------------------------------------------------
Title: Velocity Structure in the Sodium Emission from Io
Authors: Trauger, J. T.; Roesler, F. L.; Münch, G.
1976BAAS....8R.468T Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Interferometric studies of the emissions associated with Io
Authors: Münch, G.; Trauger, J.; Roesler, F.
1976BAAS....8Q.468M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Results of the infrared radiometer experiment on Pioneers 10
and 11
Authors: Ingersoll, A. P.; Muench, G.; Neugebauer, G.; Orton, G. S.
1976jsia.coll..197I Altcode: 1976IAUCo..30..197I
The infrared radiometers on the Pioneer 10 and 11 spacecraft have mapped
Jupiter in two broad spectral channels centered at wavelengths of 20
and 45 microns. Comparison of Pioneer 10 and 11 data and the results
of in-flight and laboratory calibrations indicate an absolute accuracy
of + or - 8% in the measured intensities. The relative accuracy for
comparing different regions on the planet is + or - 2%. Within the
precision of observations, the derived value of effective temperature
is independent of assumptions about the Jovian emission spectrum. The
global effective temperature is 125 + or - 3 K, implying a value of
1.9 + or - 0.2 for the ratio of planetary thermal emission to solar
energy absorbed. The effective temperatures of belts are greater than
those of zones by as much as 3.5 K. On a global scale, the poles and
equator have the same effective temperature.
---------------------------------------------------------
Title: Results of the infrared radiometer experiment on Pioneers 10
and 11.
Authors: Ingersoll, A. P.; Münch, G.; Neugebauer, G.; Orton, G. S.
1976jupi.conf..197I Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Optical identification of the supersonic emission features
in the Orion nebula.
Authors: Taylor, K.; Münch, G.
1975PASP...87..509T Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Pioneer 11 Infrared Radiometer Experiment: The Global Heat
Balance of Jupiter
Authors: Ingersoll, A. P.; Muench, G.; Neugebauer, G.; Diner, D. J.;
Orton, G. S.; Schupler, B.; Schroeder, M.; Chase, S. C.; Ruiz, R. D.;
Trafton, L. M.
1975Sci...188..472I Altcode:
Data obtained by the infrared radiometers on the Pioneer 10 and Pioneer
11 spacecraft, over a large range of emission angles, have indicated an
effective temperature for Jupiter of 125 degrees ± 3 degrees K. The
implied ratio of planetary thermal emission to solar energy absorbed
is 1.9 ± 0.2, a value not significantly different from the earth-based
estimate of 2.5 ± 0.5.
---------------------------------------------------------
Title: AZ Cassiopeiae at the 1956 - 57 eclipse.
Authors: Méndez, R. H.; Münch, G.; Sahade, J.
1975PASP...87..305M Altcode:
The spectrum of AZ Cas at the time of the 1956-57 eclipse can be
described as a combination of an F8 Ib star and a main-sequence B0-I
companion. The latter star is ejecting matter with approximately
spherical symmetry at some 50-60 km/sec, while the former has a very
extended atmosphere. The whole system seems to be also surrounded
by an expanding envelope. Determinations of the spectral type of the
red companion range from early-M, well before eclipse, to F8, in the
present material, with a Ib-luminosity class sensibly constant. This
variation is interpreted as indicating changes in the optical thickness
of the envelope surrounding the late-type companion, either intrinsic
(rho Cas episode) or related to the binary nature of the system.
---------------------------------------------------------
Title: Sodium D-Line Emission from Io: Spatial Brightness Distribution
from Multislit Spectra
Authors: Münch, G.; Bergstralh, J. T.
1975BAAS....7..386M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Pioneer 11 Infrared Radiometer Experiment: the Global Heat
Balance of Jupiter
Authors: Ingersoll, A. P.; Munch, G.; Neugebauer, G.; Diner, D. J.;
Orton, G. S.; Schupler, B.; Chase, S. C.; Ruiz, R. D.; Trafton, L. M.
1975BAAS....7..388I Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Pioneer 11 Infrared Radiometer Experiment: the Global Heat
Balance of Jupiter
Authors: Ingersoll, A. P.; Munch, G.; Neugebauer, G.; Diner, D. J.;
Orton, G. S.; Schupler, B.; Chase, S. C.; Ruiz, R. D.; Trafton, L. M.
1975BAAS....7..391I Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Highlights in planetary spectroscopy 1962 - 75.
Authors: Muench, G.
1975MSRSL...9...87M Altcode: 1975assp.conf...87M; 1975apes.conf...87M
Recent advances in spectroscopic studies of the planets with
ground-based telescopes in the photomultiplier and IR spectral ranges
are reviewed. Results of spectroscopic observations of Venus and Mars
are briefly summarized, noting that the crucial problem confronting the
interpretation of the Venusian spectrum is the nature of the clouds and
that the outstanding problem in understanding the Martian atmosphere is
the N2 or Ar concentration that may be present. Spectroscopic results
for Jupiter, Saturn, Uranus, and Neptune are discussed, emphasizing
observations of molecular hydrogen, HD, water, (C-13)H4, other
hydrocarbons, and deuterated hydrocarbons. IR and visual spectroscopic
observations of Titan and Io are reviewed which show that the CH4 bands
in Titan's spectrum are pressure broadened and that a flattened ring
of sodium is situated around Jupiter in the orbital plane of Io.
---------------------------------------------------------
Title: Multislit spectra of the sodium emission associated with Io.
Authors: Münch, G.; Bergstrahl, J. T.
1975PASP...87Q.506M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Spectrum of Neutral Oxygen in the Orion Nebula
Authors: Münch, Guido; Taylor, Keith
1974ApJ...192L..93M Altcode:
Images of the Orion Nebula in radiation of the 0 1 permitted lines are
shown to have a unique filamentary structure not apparent in the [0 1]
X6300 or other nebular lines. High-resolution profiles for these same
lines are also presented. The 0 1 X8446 structure is explained in terms
of the L resonance with the oxygen 2 3P-2 3D transition. The absence
of such filamentary structure in Ha, produced also by L decay, is
hypothesized to be the result of a concentration of solid particles in
the transition H ii-H I region of high density where fluctuations of the
0 1 X8446 emission originate. headings: line formation - Orion Nebula
---------------------------------------------------------
Title: Preliminary Infrared Radiometry of the Night Side of Mercury
from Mariner 10
Authors: Chase, S. C.; Miner, E. D.; Morrison, D.; Munch, G.;
Neugebauer, G.; Schroeder, M.
1974Sci...185..142C Altcode:
The infrared radiometer on Mariner 10 measured the thermal emission from
the planet with a spatial resolution element as small as 40 kilometers
in a broad wavelength band centered at 45 micrometers. The minimum
brightness temperature (near local midnight) in these near-equatorial
scans was 100 degrees K. Along the track observed, the temperature
declined steadily from local sunset to near midnight, behaving as would
be expected for a homogeneous, porous material with a thermal inertia of
0.0017 cal cm<SUP>-2</SUP> sec<SUP>-1/2</SUP> degrees K<SUP>-1</SUP>,
a value only slightly larger than that of the moon. From near midnight
to dawn, however, the temperature fluctuated over a range of about 10
degrees K, implying the presence of regions having thermal inertia
as high as 0.003 cal cm<SUP>-2</SUP> sec<SUP>-1/2</SUP> degrees
K<SUP>-1</SUP>.
---------------------------------------------------------
Title: Mariner Venus/Mercury: Results of Infrared Radiometer
Experiment
Authors: Munch, G.
1974BAAS....6S.386M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Results from the Infrared Radiometer Experiment on Pioneer 10
Authors: Münch, G.; Neugebauer, G.; Schroeder, M.; Trafton, L.;
Chase, S. C.; Ruiz, R.
1974BAAS....6..388M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Preliminary Infrared Radiometry of Venus from Mariner 10
Authors: Chase, S. C.; Miner, E. D.; Morrison, D.; Munch, G.;
Neugebauer, G.
1974Sci...183.1291C Altcode:
The intensity of emission at 45 micrometers, measured with high spatial
resolution along a single crossing of the Venus disk, is presented. On
the average, the observed darkening toward the limb varies nearly
linearly with the cosine of the emission angle. The brightness
temperature, extrapolated to normal emission, is 255 degrees K. The
limb darkening curve, interpreted in a linear approximation, implies
that the atmosphere is quite opaque, with an absorption coefficient of
0.24 per kilometer. Changes in curvature present in the limb darkening
curve suggest the existence of thermal inhomogeneities with scale
comparable to that of the dark markings shown by ultraviolet images.
---------------------------------------------------------
Title: Pioneer 10 Infrared Radiometer Experiment: Preliminary Results
Authors: Chase, S. C.; Ruiz, R. D.; Munch, G.; Neugebauer, G.;
Schroeder, M.; Trafton, L. M.
1974Sci...183..315C Altcode:
Thermal maps of Jupiter at 20 and 40 micrometers show structure
closely related to the visual appearance of the planet. Peak brightness
temperatures of 126 degrees and 145 degrees K have been measured on
the South Equatorial Belt, for the 20- and 40-micrometer channels,
respectively. Corresponding values for the South Tropical Zone are
120 degrees and 138 degrees K. No asymmetries between the illuminated
sunlit and nonilluminated parts of the disk were found. A preliminary
discussion of the data, in terms of simple radiative equilibrium models,
is presented. The net thermal energy of the planet as a whole is twice
the solar energy input.
---------------------------------------------------------
Title: Announcement
Authors: Jascheck, C.; Giclas, H. L.; Hayford, P.; Johnson, H. L.;
Landolt, A. U.; Luyten, W.; Marlborough, J. M.; Mermilliod, J. -Cl.;
Münch, G.; Stephenson, C. B.; Wallerstein, G.
1973BICDS...5...26J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Helium Abundance on Jupiter (Article published in the Space
Science Reviews special issue on 'Outer Solar System Exploration -
An Overview', ed. by J. E. Long and D. G. Rea.)
Authors: Hunten, Donald M.; Münch, Guido
1973SSRv...14..433H Altcode:
Methods of determining helium on Jupiter (and the Jovian planets)
are critically surveyed. Current information is consistent with
solar abundance, He/H<SUB>2</SUB> = 0.11 by number. The available
lines of evidence are the mean density, spectral-line broadening, and
stellar occultations. Methods usable from spacecraft flying by are
discussed. Observation of far-infrared emission has great promise,
but we may have to await the development of entry probes for the
greatest assurance.
---------------------------------------------------------
Title: On the Spectrum of Titan
Authors: Münch, Guido
1973BAAS....5..305M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A strategy for investigation of the outer solar system. Outer
planets, their satellites, and particles and fields at great distances
from the sun.
Authors: Münch, G.; Hunten, D. M.; Kliore, A. J.; Lewis, J. S.;
McElroy, M. B.; Spencer, N. W.; Stone, P. H.; Wetherill, G. W.;
Cameron, A. G. W.; Hubbard, W. B.; Murray, B. C.; Peale, S. J.; van
Allen, J. A.; Axford, W. I.; Gulkis, S.; Kennel, C. F.; Montgomery,
M. D.; Parker, E. N.; Sonett, C. P.; Stone, R. G.; Trainor, J. H.;
Rea, D. G.; Long, J. E.; Padrick, B. D.
1973SSRv...14..347M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Preliminary report on infrared radiometric measurements from
the Mariner 9 spacecraft.
Authors: Kieffer, H. H.; Chase, S. C., Jr.; Miner, E.; Münch, G.;
Neugebauer, G.
1973JGR....78.4291K Altcode:
Preliminary 10- and 20-μm brightness temperatures of Mars are
presented. More than 35% of the Martian surface was observed with
a resolution better than 100 km. On the whole, the results confirm
the thermal properties derived from the Mariner 6 and 7 radiometers,
although the temperatures, on the average, were cooler and shifted with
respect to the Martian day during the dust storm. Thermal inertias and
radiometric albedos were derived for many areas; no clear correlation
exists between these properties. Thermal structure again was found at
the spatial limit of the radiometer; no cases were found in which it
was necessary to invoke internal heat sources.
---------------------------------------------------------
Title: High resolution astronomical spectroscopy: its future.
Authors: Muench, G.
1972ailt.conf...21M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Infrared Thermal Mapping Experiment: The Viking Mars Orbiter
Authors: Kieffer, Hugh H.; Neugebauer, G.; Munch, G.; Chase, S. C.,
Jr.; Miner, E.
1972Icar...16...47K Altcode:
The Mars infrared thermal mapper (IRTM) will be carried on the scan
platform of the orbiter of the Viking 1975 mission. The IRTM is a
multichannel radiometer with several detectors in each of six spectral
regions. This instrument will measure the reflected solar radiation and
surface thermal emission from the area viewed by the orbiter imaging
system with nominal 5 km resolution. Extensive additional areas will
be covered for which simultaneous imaging will not be available. The
spectral channels are selected to be sensitive to surface emissivity
variations and provide good temperature resolution over the entire range
of Martian temperatures. These observations will allow determination
of the surface kinetic temperature and thermal balance, and by coverage
of the dark hemisphere, a search for regions with anomalous cooling can
be made. Observations of ground frosts or clouds will help to determine
their composition, and in the case of extensive H <SUB>2</SUB>O frosts,
will allow the local water vapor pressure to be estimated.
---------------------------------------------------------
Title: Mariner 9 Science Experiments: Preliminary Results
Authors: Steinbacher, R. H.; Kliore, A.; Lorell, J.; Hipsher, H.;
Barth, C. A.; Masursky, H.; Munch, G.; Pearl, J.; Smith, B.
1972Sci...175..293S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Infrared Radiometry Experiment on Mariner 9
Authors: Chase, S. C., Jr.; Hatzenbeler, H.; Kieffer, H. H.; Miner,
E.; Munch, G.; Neugebauer, G.
1972Sci...175..308C Altcode: 1972Sci...175..398C
The brightness temperatures at 10 and 20 micrometers measured by the
Mariner 9 infrared radiometer differ substantially from those predicted
by the radiometer results of Mariners 6 and 7. The results indicate
a significant latitude-dependent contribution of the atmospheric dust
to the observed thermal emission.
---------------------------------------------------------
Title: Jupiter: An Unidentified Feature in the 5-Micron Spectrum of
the North Equatorial Belt
Authors: Munch, G.; Neugebauer, G.
1971Sci...174..940M Altcode:
Grating spectra of the North Equatorial Belt of Jupiter between 4.5
and 5.1 microns, obtained with a nominal resolving power of 180, are
presented. An absorption feature centered at 4.73 microns and not due
to a known constituent has been found. Its possible identification
is discussed.
---------------------------------------------------------
Title: Mariner 1969 Infrared Radiometer Results: Temperatures and
Thermal Properties of the Martian Surface
Authors: Neugebauer, G.; Münch, G.; Kieffer, H.; Chase, S. C., Jr.;
Miner, E.
1971AJ.....76..719N Altcode:
The reduced data of the Mariner 6 and 7 Infrared Radiometer Experiments
are presented, along with a discussion of the reduction and calibration
procedures. Evidence is presented showing that the surface of Mars is
strongly nonhomogeneous in its thermal properties, on scales ranging
from those of the classical light and dark areas to the limit of
resolution of the radiometers. On the sunlit side, the mean thermal
inertia, for admissible bolometric albedos, is 0.006 (cal cm sec
0K-1). The dark areas Syrtis Major and Mare Tyrrhenum, observed at
night, require thermal inertias as high as 0.010. The temperatures
measured over the circular basin Hellas require a bolometric albedo of
0.40 and also a high thermal inertia. The temperature measured over the
south polar cap, 148 K, provides evidence that the major constituent
of the frost deposit is CO2.
---------------------------------------------------------
Title: The Distribution of Gas and Dust in the Orion Nebula
Authors: Münch, G.; Persson, S. E.
1971ApJ...165..241M Altcode:
Photoelectric measurements of Balmer-line intensities at 4000 points
on the Huyghenian region of the Orion Nebula, with an angular
resolution of 3 arc sec, are analyzed to show the following: (1)
The differential reddening that affects nebular radiation can be
accounted for only if dust particles are mixed with the ionized gas
and the wavelength dependence of the dust-absorption coefficient is
the same as that determined for the Trapezium stars. (2) The intensity
and reddening gradients, on the average, have the same sign. This fact
indicates that dust is well mixed with the gas and that, statistically,
fluctuations in gas density are positively correlated with variations
in dust density. The behavior of the intensities of the He I lines at
10830, 7065 and 5876 A, measured at 150 points covered by Balmer-line
observations, can be understood only if dust, absorbing resonantly
trapped X10830 photons, is mixed with the gas.
---------------------------------------------------------
Title: The Distribution of Gas and Dust in the Orion Nebula
Authors: Münch, G.; Persson, S. E.
1971BAAS....3...17M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Mariner 1969: Results of the Infrared Radiometer Experiment
Authors: Münch, G.; Neugebauer, G.; Chase, S. C.
1971IAUS...40..258M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected Topics on the Physics of the Interstellar Medium
Authors: Münch, G.
1970gaas.conf..191M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Infrared Radiometry Experiment for Mariner Mars 1971
Authors: Chase, S., Jr.; Miner, E.; Münch, G.; Neugebauer, G.
1970Icar...12...46C Altcode:
The infrared radiometer is designed to provide brightness temperatures
of the surface of Mars by measuring the energy radiated in the 8 to
12 and 18 to 25 μ wavelength bands. The instrument is essentially the
same as that flown on the Mariner Mars 1969 missions, modified only to
define more sharply the field of view. Because Mariner Mars 1971 will
orbit Mars, a given area of the planet will be observed at a variety
of local times, and the characterization of the various areas by their
thermophysical properties will be more complete than that obtained by
Mariner Mars 1969.
---------------------------------------------------------
Title: Interstellar Gas
Authors: Münch, G.
1970saac.book..295M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Appearance of Jupiter in the thermal infrared.
Authors: Münch, G.; Neugebauer, G.
1970TrAGU..51..771M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Mariner 1969: Preliminary Results of the Infrared Radiometer
Experiment
Authors: Neugebauer, G.; Munch, G.; Chase, S. C., Jr.; Hatzenbeler,
H.; Miner, E.; Schofield, D.
1969Sci...166...98N Altcode:
The thermal energy emitted by Mars was measured in the 8- to 12- and 18-
to 25-micrometer bands. The minimum temperature derived for the southern
polar cap is 150 degrees K, an indication that the cap is formed by
frozen carbon dioxide. No significant temperature fluctuations were
detected with a 100-kilometer scale.
---------------------------------------------------------
Title: The structure of the atmospheres of the major planets.
Authors: Trafton, L. M.; Münch, G.
1969JAtS...26..813T Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Internal Motions in the Planetary Nebula NGC 6543
Authors: Münch, Guido
1968IAUS...34..259M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Interstellar Absorption Lines
Authors: Münch, Guido
1968S&SS....7..365M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Small-Scale Thermal Homogeneity of the Orion Nebula
Authors: Münch, Guido
1968iih..conf..507M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Interstellar Absorption Lines
Authors: Münch, Guido
1968nim..book..365M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The physical state of the interstellar gas in the Messier
31 nucleus
Authors: Munch, G.
1968IAUS...29...71M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Infrared Coronal Lines. II. Observation of [SI x] λ 1.43 μ
and [Mg VIII] λ 3.03&mu
Authors: Münch, G.; Neugebauer, G.; McCammon, D.
1967ApJ...149..681M Altcode:
The wavdengths and intensities of the coronal lines of the ions Si +
and Mg8+, resulting from the airborne observation of the November 12,
1966, total solar eclipse, are given
---------------------------------------------------------
Title: Spectrophotometry of Uranus from 3300 to 11000 Angstroms
Authors: Younkin, R. L.; Munch, G.
1967AJ.....72R.328Y Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observation of the coronal lines of [Si X] and [Mg VIII]
at the 12 November 1966 Solar eclipse
Authors: Munch, G.; Neugebauer, G.; McCammon, D.
1967AJ.....72S.313M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Infrared Spectra of Low-Temperature Stars
Authors: McCammon, D.; Munch, G.; Neugebauer, G.
1967ApJ...147..575M Altcode:
Spectra of stars of types M, N(R), and S, as well as of NML objects
in Cygnus and Taurus, are presented in the regions 5-1.8 and x1 9-2 5
. In M stars the absorption due to stellar H2O is apparent from the
wings of the bands at xl .4, xt .9, and x2.7 Stars of N and S types
show weaker H2O absorption. The Av = 2 and Av = 3 vibration-rotation
band sequences of CO appear well marked in all stars, being somewhat
weaker in the M types than in other stars. The late N stars Y CVn and
U Hyd show a sharp discontinuity or band head at xl .76 not present
in other stars. The entire spectra of Y CVn and U Hyd shortward of
this discontinuity appears veiled, the Av = 3 CO band sequence being
conspicuously weak. The spectra of the NML objects in Cygnus and
Taurus have spectral characteristics resembling the carbon more than
the M stars.
---------------------------------------------------------
Title: The Weakness of Helium Lines in Globular Cluster and Halo
B Stars
Authors: Greenstein, Jesse L.; Münch, Guido
1966ApJ...146..618G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Absorption Lines from Intermediate-Latitude Interstellar
Complexes
Authors: Münch, Guido
1966PASP...78..305M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Infrared Lines of the Solar Corona. I. Prediction
Authors: Münch, Guido
1966ApJ...145..237M Altcode:
The existence of coronal lines in the instrumental infrared, due to the
ions Mg7+, Al8+, and 5i8+ and Si +, is predicted and their intensities
are estimated. The possibility of detecting these lines with practicable
infrared spectrometers and photoconductive detectors is analyzed, taking
into consideration attenuation by atmospheric gases. The powers radiated
in the [Mg viiij, [Si ix], and [Si x] lines are found to be large
enough to make their detection feasible with instruments of modest size.
---------------------------------------------------------
Title: Caltech-JPL Lunar and Planetary Conference
Authors: Brown, Harrison; Stanley, Gordon J.; Muhleman, Duane O.;
Münch, Guido
1966lupl.conf.....B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: High-Resolution Observations of Interstellar Sodium D Lines
with an Interferometer.
Authors: Vaughan, Arthur H., Jr.; Münch, Guido
1966AJ.....71..184V Altcode:
Interstellar sodium D line profiles in some 20 early-type stars were
scanned at a resolving limit of about 18 mA with a single-etalon
Fabry- Perot interferometer. The coude' spectrum scanner of the
100-in. telescope was tised as a premonochromator, a monitor channel at
nearby ~`avelengths provided seeing compensation, and pulse Counting
techniques were employed. The method achieves an efficiency gain of
a factor 10 compared to conventional spectroscopy for the study of
the D lines. The faintest star of this survey (HD 217101, `B4~=6.2)
gave a signal-to-dark ratio of 3. In at least one-half of the stars
observed the number of Na I components resolved interferometrically
exceeded the number of Ca II components previously reported by
W. S. Adams (Astrophys. J. 109, 335, 1949). In most cases the use of
higher resolution is responsible, but it is also of interest that a
few components were found in Na I which are weak or missing in Ca II,
in contrast to previous studies (Routly and Spitzer, Astrophys. J. 115,
227, 1952) where the inverse has usually been true. A comparison of our
data for a Cygni with results obtained by a different interferometric
technique by L. M. Hobbs (Astrophys. J. 142, 160, 1965) indicates
some discrepancies which as yet are unexplained. This work is partly
supported by the National Aeronautics and Space Administration under
Grant NsG-426.
---------------------------------------------------------
Title: Predicted Coronal Lines in the Instrumental Infrared.
Authors: Münch, Guido
1966AJ.....71..173M Altcode:
The ions Mg7+, Al5+, 5j9+, with 2s22p ground state configurations and
ionization potentials IP of 266, 330, and 401 eV, produce coronal
lines at wavelengths near 3.032, 2.047, and 1.431 p. The ion Si~+
with 2s22p2 ground state and IP=351 eV produces lines at 2.587 and
3.859 p. An estimate of the strength of these coronal lines has been
made on the basis of assumed abundances and approximate theories of
ionization and excitation. It has been found that the lines of Mg7+,
Si5+, and 5j9+ should be as strong as the iron coronal lines in the
photographic region. In consideration of the detectivity of infrared
detectors (PbS), estimates have been made of the signal to noise ratios
that may be reached with optics of practical size during a total solar
eclipse. The effects of atmospheric absorption have been taken into
account to the extent justified by the uncertainties affecting the
predicted wavelengths of the lines. The probability that the lines
will be observable from ground notwithstanding atmospheric absorption
and that they can be detected appear fairly high.
---------------------------------------------------------
Title: Visible and Near-Infrared Spectrophotometry of Saturn's Rings.
Authors: Younkin, Robert L.; Münch, Guido
1966AJ.....71R.188Y Altcode:
Measurements of the narrow-band spectral energy distribution of the
rings of Saturn have been made at the Mount Wilson Observatory using
the 60-in. reflector and the Fastie- Ebert spectrometer. Spectral scans
from 0.51 to 1.1 IL were made of a segment of the rings at the western
end of the semimajor aXls. The energy distribution was determined at 54
points in this wavelength region. The color sensitivity of the system
was determined from scans of a Lyr and the a Lyr energy distribution
of Oke. The relative reflectance of the rings was calculated by use of
the solar intensity values of Labs and Neckel, converted to solar flux
by the ratios of Minnaert. The reflectance of the rings is very nearly
constant from 0.78 to 1.05 IL Shortward of this region it falls slowly
to 0.60 IL' then more rapidly to a value at 0.51 IL some 0m.45 below
the maximum. There is a slight decrease in reflectance (0~~03~0m.0S)
from 1.05 to 1.08 IL This is marginally outside of the experimental
error. Owen has recently reported a drop in the reflectance of the
rings from 1.04 to 1.09 IL' whid~ he identified as due to water
ice. This drop was determined on the basis of a drop in the ratio
of the intensity of the rings to the intensity of Saturn in this
region. Separate measurements at Mount Wilson of the reflectance of
Saturn show a continuous strong absorption from 0.97 to 1.04 IL This
unfortuitous coincidence yields a large drop in the ratio beyond 1.04
IL which will completely mask any possible ice absorption which by
the results above will be only a few percent at most.
---------------------------------------------------------
Title: Structure and Kinematics of the Orion Nebula
Authors: Munch, G.
1966IAUTB..12..463M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Spectra of Two Extremely Red Objects.
Authors: Münch, Guido; Scargle, Jeffrey D.
1965ApJ...142..401M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Galactic Structure and Interstellar Absorption Lines
Authors: Münch, Guido
1965gast.book..203M Altcode: 1965S&SS....5..203M; 1965gast.conf..203M
No abstract at ADS
---------------------------------------------------------
Title: On the interpretation of strong CO<SUB>2</SUB> absorption
bands in the spectrum of Mars / G. Munch and G. Neugebauer
Authors: Munch, Guido; Neugebauer, Gerry
1965LowOB...6..181M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Wavelength Dependence of the Band Structures of Jupiter and
of Saturn.
Authors: Younkin, Robert L.; Münch, Guido
1964AJ.....69..565Y Altcode:
Photoelectric measurements of the band structures of Jupiter and of
Saturn were made during September 1963 by moving a small slot along
the central meridian of the planetary image. The Mt. Wilson Ebert
spectrometer was used on the 60-in. reflector as a monochromator
to select wavelengths from X3200 A to 10400A. Curves obtained for
Saturn show: (1) radiance of both equatorial zone and north tropical
zone relative to B-ring exhibit broad maxima in X5800 - X7500 range,
falling sharply to an ultraviolet minimum near X3800 A; (2) radiance
of equatorial zone relative north tropical zone is slightly greater
than unity beyond X6000 A, but falls to 0.58 in the ultraviolet. This
ratio ~ecomes large in str9ng CH4 bands: 1.6 at X7270 A and 3.7 at
X8912A with a fairly sharp discontinuity at the north equatorial
belt. Consistent with these observations is an atmospheric model in
which cloud particles over the entire planet possess similar selective
absorption which increases with decreasing wavelength below X5200A,
but a lower effective cloud level in the temperate and polar regions'
than the equatorial zone. Thus at short wavelengths where Rayleigh
scattering dominates particle scattering, the temperate and polar
regions are brighter than the equatorial zone; and, conversely, at long
wavelengths and particularly in the CH4 bands, where particle scattering
dominates. For Jupiter, the north tropical zone was the brightest region
of the planet throughout the range of wavelengths. Its radiance relative
to the south tropical zone is anomalous in CH4 absorption, increasing
in the X8900 A band, and decreasing in the X7270 A band. Contrast
between tropical zones and adjacent equatorial belts increases with
decreasing wavelength below X5500 A. In strong CH4 absorption bands the
limb darkening with latitude greatly increases. The south equatorial
belt becomes the brightest region of the' planet. In the X8900 A band
both polar regions become bright at the limb.
---------------------------------------------------------
Title: Radial Velocities of Distant OB Stars.
Authors: Münch, Guido; Münch, Luis
1964ApJ...140..162M Altcode:
The results of radial-velocity measurements for twenty-seven faint
OB stars at galactic longitudes between 1" - 18 and 1" = 66 are
presented. On the basis of spectroscopic absolute magnitudes in the
Yerkes system and UB V photometry, the rotational velocities of the
stars around the galactic center have been derived. In comparison with
the rotational curve indicated by the interstellar neutral hydrogen, the
stellar motions suggest rotational velocities lower by about 25 km/sec
at distances from the center around half that of the Sun. The general
shape of the rotation-curve provided by the new stellar observations
remains thus the same as it was found in our previous study.
---------------------------------------------------------
Title: An Interstellar Cloud with a High Concentration of CN
Molecules.
Authors: Münch, Guido
1964ApJ...140..107M Altcode:
A group of stars embedded in an emission nebula near the cluster
NGC 7822 has been discovered to have a unique interstellar spectrum,
characterized by exceedingly strong CN lines. Evidence is presented
favoring the hypothesis that the CN molecules arise in the immediate
neighborhood of the H ii region boundary. It is further suggested that
the CN molecules are formed in the solid particles of the H 1 region
when flashed by the UV radiation in the advancing ionization front.
---------------------------------------------------------
Title: An Analysis of the Spectrum of Mars.
Authors: Kaplan, Lewis D.; Münch, Guido; Spinrad, Hyron
1964ApJ...139....1K Altcode:
On a high-dispersion spectrogram of Mars taken at Mount Wilson
rotational lines of 1120 near X 8300 and CO2 near x 8700 have been
detected. Recent laboratory measurements of line strengths by D Rank
have been used to determine the amounts of H2O and CO2 in the atmosphere
of Mars: t4 + 7 precipitable water and 55 + 20 m atm CO2. From the
absence of O2 in the Martian spectra, we set an upper limit of 70
cm atm for the O2 content. By suitably combining the CO2 amount with
observations by Kuiper and Sinton of the strongly saturated bands in
the 2-j# region, a surface pressure of 25 + 15 mb has been derived. The
implications of the results on the composition of the Martian atmosphere
are discussed.
---------------------------------------------------------
Title: Molecular Absorptions and Color Distributions over Jupiter's
Disk.
Authors: Münch, Guido; Younkin, Robert L.
1964AJ.....69R.553M Altcode:
Absorptions of NH3 and CH4 and energy curves of Jupiter have
been obtained with a photoelectric scanning spec- trometer at the
60-in. Mt. Wilson reflector. Spectrum scans at various parts of the
disk and surface scans at fixed wavelength have been obtained with
resolving powers around 10 A in the range 0.55-1.1 p. The behavior of
individual lines or bands has also been studied photographically in
Coude' spectra. Up to date the following results have been obtained:
(a) The quadrupole H2 lines of the (3,0) vibrational band do not show
detectable variation in strength with longitude or latitude. (b)
The zones have a bluer spectrum and show more limb darkening than
the belts. (c) The absorption at the very strong band X8892 A (CH4)
increases markedly with latitude and appears stronger in zones than in
belts. At the polar caps bright cusps are observed. (d) Absorption in
the weak NH3 X6450 A and CH4 X6190 A bands is slightly weaker in belts
than in zones, and at fixed latitude decreases in strength both towards
the morning and evening limbs. This effect is well marked also in the
lines of the NH3 X7900 band. From (a) it is inferred that, above the
layers showing visual structure, there is sufficient gas to produce
completely saturated H2 lines, the strength of which, then cannot
provide information about the relative abundance of H2 with respect
to other constituents. Result (b) suggests that, above the zones,
Rayleigh scattering plays a larger role in the diffuse reflection
of solar light than above the belts. The red color of the zones,
relative to the sun, still indicates the presence of selectively
scattering solid particles, which need not differ in chemical or
physical composition from the particles forming the cloud belts. The
higher effective layer for reflection in the belts is also indicated
by (a). The polar brightening reveals the existence of an extremely
high cloud cap, or possibly frozen CH4. Previous results of Hess agree
qualitatively with (d). The intensity variation in longitude of the
lines can be understood in terms of the pressure dependence of the
absorption coefficient in lines arising by diffuse reflection.
---------------------------------------------------------
Title: H<SUB>2</SUB>O and CO<SUB>2</SUB> Absorption in the
Photographic Infrared Spectrum of Mars
Authors: Münch, G.; Kaplan, L. D.; Spinrad, H.
1963PASP...75..416M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Nebular absorption of He 3889 A.
Authors: Munch, G.; Wilson, O. C.
1963AJ.....68..287M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Letter to the Editor: the Detection of Water Vapor on Mars.
Authors: Spinrad, Hyron; Münch, Guido; Kaplan, Lewis D.
1963ApJ...137.1319S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Spectrum of Saturn
Authors: Munch, G.; Spinrad, H.
1963LIACo..11..541M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Nebular Absorption of He I λ3889.
Authors: Münch, G.; Wilson, O. C.
1963AJ.....68Q.287M Altcode:
The presence of an absorption line arising from the 2~5 metastable
level of neutral helium in the spectra of the stars imbedded in the
Orion Nebula was noticed long ago by 0. C. Wilson. Lately it has been
shown by G. Mu~nch and 0. C. Wilson (Z. Astrophys. 56, 127, 1962)
how the strength of this nebular absorption line may be related to
the surface brightness of a homogeneous emission nebula. The lack
of agreement between the surface brightness thus computed for the
Orion Nebula with the observed value, has been interpreted in terms
of density inhomogeneities in the nebula, independently postulated
by Osterbrock on other grounds. Because this interpretation has been
criticized by K. Wurm (Z. Astrophys. 52,149, 1961), new observational
evidence related to the line in question is being obtained. In this
communicatioi~, besides new data for the Orion stars, the results
of the search for the absorption line in other emission nebulae are
presented. So far the line has been detected in a number of stars in
the complex M8- M20, in BD +6601675, exciting NGC 6822, in BD +6002522
exciting NGC 7635, and in HD 64315, exciting star of NGC 2467. The stars
imbedded in 20 other H II regions do not have detectable He I nebular
absorption. Although a complete discussion of the data requires surface
brightness determinations (corrected for interstellar and internebular
extinction) not available yet, it is shown how the recent observations
fully support the interpretation advanced earlier by Wilson and Mu~nch.
---------------------------------------------------------
Title: The Intensity of Forbidden Emission Lines.
Authors: Münch, Guido
1962ApJ...136..823M Altcode:
A general formula for the intensity of a forbidden emission line in a
two-level atom is derived, taking into consideration induced emissions,
saturation effects, and departures from a Boltxmann distribution. The
kinetic temperature is supposedly given, but not necessarily is it taken
as constant It is shown how this general formula embodies expressions
used in the past separately for the optical, infrared, and radio regions
of the spectrum As an example of application of the formulae derived,
the emission rate in the fine-structure transition of the ground state
of C+ is re-evaluated under the conditions prevailing in interstellar
H I regions As an illustration of a line arising in a medium with
variable temperature, the intensity in the normal direction and flux
of the line arising between the lowest two fine-structure levels of
the ground state of oxygen is computed, under conditions appropriate
to the earth's upper atmosphere. It is found that the outward energy
flux in this line compares with the energy input provided by solar
X-rays at the time of low solar activity.
---------------------------------------------------------
Title: Interstellar Gas Near the Sun.
Authors: Münch, G.; Unsöld, A.
1962ApJ...135..711M Altcode:
Observations of interstellar Ca ii lines in the spectrum of the nearby
star a Oph and other stars in the same area of the sky are reported
From the radial velocities and intensities of the interstellar lines
it is shown that the cloud in front of a Oph has linear dimensions of
the order of 1 pc and a total number density of order unity
---------------------------------------------------------
Title: Recent Spectroscopic Investigations of Jupiter and Saturn.
Authors: Spinrad, Hyron; Münch, Guido; Trafton, Laurence M.
1962AJ.....67Q.587S Altcode:
This report deals with high-dispersion spectroscopic studies currently
in progress at the Mt. Wilson and Palomar Observatories. On spectra
taken with the slit along Jupiter's equator we have found that the
inclinations of the Jovian ammonia and methane absorption lines are less
than would be expected if these gases rotate with the planet (Spinrad,
Astrophys. J., to be published, 1962). The result is interpreted to mean
a slow rotation for the NH3 and CH4 molecules. In the case of Saturn,
the CH4 lines are inclined so that the methane appears to be rotating
about 10% faster than the cloud layer producing the scattered Fraunhofer
spectrum (Munch and Spinrad, 11th Liege Symposium, Physics of Planets,
1962). The Jovian NH3 lines vary in strength with time, probably on a
time scale longer than a few days. From the half-widths of the Jovian
NH3 and CH4 absorption lines we have determined crude upper limits for
the total pressure in this portion of Jupiter's atmosphere. Three weak,
sharp new absorption lines not associated with the methane or ammonia
bands were found in the Jovian spectrum; one of these is the 5(1)
line of H2 in the (4,0) band. No reasonable coincidences have been
established for the other two unidentified features. On Saturn we have
found both the 5(1) and 5(0) lines of molecular hydrogen in the (4,0)
band. The total amount of H2 visible is comparable to the amount above
the Jovian "reflecting layer"; a rotational temperature for the H2
has been determined. We cannot identify any of the red NH3 lines in
the Saturn spectrum with certainty. The ammonia content of Saturn's
atmosphere in 1962 must be considerably below the usually quoted value
of 200 cm-atm.
---------------------------------------------------------
Title: Structural Problems of Galaxies in the Light of LYMAN-α
Authors: Münch, Guido
1962saa..conf..219M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Structure of the Orion Nebula. A Reply to K. WURM. With
2 Figures in the Text
Authors: Münch, G.; Wilson, O. C.
1962ZA.....56..127M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Motions of the Interstellar Gas in the Central Regions
of Galaxies
Authors: Münch, Guido
1962IAUS...15..119M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Interstellar Matter at Large Distances from the Galactic Plane.
Authors: Münch, Guido; Zirin, Harold
1961ApJ...133...11M Altcode:
The interstellar gas at large distances z from the galactic plane
is studied by the absorption lines it produces on the spectrum of
distant stars off the Milky Way. From the statistics of multiple lines
in various ranges of z, it is shown that some gas clouds probably
exist at z = 1 kpc. The number of clouds observed in 0 5 <z <
1 kpc has been found to be larger than would be expected from the
known distribution of their velocity components in the galactic
plane. The apparent asymmetry in the distribution of high-velocity
clouds is explained as the result of decreased chances of collisions
in the z-direction and also in terms of an intrinsic anisotropy in the
mechanism accelerating the clouds. The typical time required for the
clouds to reach their actual probable height from z = 0 is evaluated
to be 40 X 106 years From the line intensities and by assuming cosmic
abundance of the elements, a relation between the linear dimensions and
the densities of the clouds is established. Irrespective of whether
the clouds are H I or H ii regions, it is found that their continued
existence for 40 X 106 years requires the operation of a process
preventing them from expanding. The physical conditions prevailing
in a galactic halo or corona exerting pressure on the clouds are
next analyzed. It is shown how the observations rule out a halo with
an electron temperature T, around 10 K. A corona with T = 106 K, as
postulated by Spitzer, on the other hand, is found admissible, provided
that the high-velocity clouds at high z are H ii regions. The large
energy input by conduction from the corona may be balanced by radiative
losses only at about T - 10 K. Next the ionization e uilibrium in the
clouds is briefly discussed, and it is suggested that the anomalous
abundance ratio Na Ca observed in interstellar space is the result of
using an unrealistic mean stellar radiation field in the photoionization
computations. In this context, the results of a calculation of the
ionization equilibrium of aluminum is presented It is shown that the Al
I line at X 3964 should have a strength about one-twentieth that of Ca
I X 4226. In a final section the possible mechanisms by means of which
interstellar clouds may be accelerated are discussed. It is shown how
the operation of the Oort-Spitzer process requires a ratio between the
total amounts of ionized and neutral interstellar matter much larger
than is observed. The relevance of magnetic fields in accelerating
small masses of ionized field4ree material is thereby emphasized.
---------------------------------------------------------
Title: The Linear Dimensions of HII Regions.
Authors: Münch, Guido
1960AJ.....65..495M Altcode:
The ionization equilibrium of interstellar hydrogen near hot stars has
been studied and has taken into consideration the finite probability
for recombination in the ground state. Simultaneous solutions of the
transfer equation for radiation beyond the head of the Lyman series
and Saha's relation have been found, paying attention to the spherical
geometry. For a value ~=0.4 for the probability of scattering of an UV
quantum, it is found that the radius of the sphere of ionized hydrogen
increases by a factor of 1.6 with respect to that obtained neglecting
the diffuse radiation field (Stromgren's radius). These results are
in disagreement with those derived by Pottash and Jefferies (1959,
Ann. dAstrophys. 22, 297) owing to an erroneous boundary condition
adopted by these authors. In considering the case of a thin spherical
shell around the hot star, Pottash and Jefferies impose as boundary
condition at the inner boundary the vanishing of the diffuse radiation
field. The correct boundary condition is the vanishing of the flux of
diffuse radiation throughout the inner volume enclosed by the shell
(Milne's "planetary nebula" condition). The numerical integrations
and procedures followed by Pottash and Jefferies for the spherical
case have not been published in sufficient detail to be compared with
our results. It is suspected that their work for this case is also
vitiated by the use of a boundary condition with no physical meaning.
---------------------------------------------------------
Title: On the Rotation of the Inner Parts of the Galactic System.
Authors: Münch, Guido; Münch, Luis
1960ApJ...131..253M Altcode:
Results of radial-velocity measurements for 18 distant OB stars in
galactic longitudes between 345 and 35 are presented. On the basis
of published spectroscopic distance moduli, the results have been
interpreted in terms of rotational velocities around the galactic center
and compared with those of the interstellar neutral hydrogen. The
stellar motions seem to suggest for the rotational velocity of the
galactic system, at a distance of 6 kpc from the center, a value 10
km/sec higher than that indicated by the 21-cm line. At a distance
of 4 kpc from the center, the stellar motions provide rotational
velocities around 25 km/sec lower than the 21-cm line profiles do. This
discrepancy is shown to be unlikely to arise from systematic errors
in the spectroscopic distance moduli or in the radial velocities. The
motion of the stars considered indicates a value for Oort's constant
A somewhat larger than the classical value A = 20 km/sec. The BO.S
Ia star HD 173438 has been found to be a single-line spectroscopic
binary with a 250- day period, a semiamplitude of 50 km/sec, and an
eccentricity of 0.54.
---------------------------------------------------------
Title: On the interpretation of the spiral structure in the galactic
system
Authors: Münch, G.
1960AnAp...23..403M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Motions of the Gas near the Nucleus of M31.
Authors: Münch, Guido
1960AJ.....65R..55M Altcode:
Some results of the observation of [0113 emission in the neighborhood
of the nucleus of the Andromeda Nebula are presented. With the prime
focus spectrograph of the Hale reflector at a dispersion of 66 A/mm,
the [0113 doublet at ~3726-28 has been resolved and detected out to
a distance of 50" from the nucleus, with the slit at various position
angles. While the individual components of the doublet appear narrow,
they show sudden large variations in velocity superposed on the
rotational pattern of the system as a whole. Because of the underlying
absorption spectrum, the true value of the velocities can not yet be
found accurately, but, on the whole, the motion of the gas seems to have
a well-defined outward motion, amounting to 50 km/sec at a distance
of 200 pc from the nucleus. The noncircular nature of the motion
is most clearly observed with the slit along the minor axis, where
all rotational effects should vanish. There are reasons to interpret
these observations in terms of motions taking place predominantly in
directions confined to the symmetry plane of the system.
---------------------------------------------------------
Title: The Theory of Model Stellar Atmospheres
Authors: Münch, Guido
1960stat.book....1M Altcode: 1960S&SS....6....1M; 1960stat.conf....1M
No abstract at ADS
---------------------------------------------------------
Title: Letter to the Editor Expending Motions of Interstellar Gas
in the Nuclear Region of Messier 31.
Authors: Münch, Guido
1960ApJ...131..250M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A New O-Type Subdwarf.
Authors: Münch, Guido; Slettebak, Arne
1959ApJ...129..852M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Distance of the Cassiopeia Radio Source.
Authors: Münch, Guido; Münch, Luis
1959ApJ...129..854M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Mass-Luminosity Ratio in Stellar Systems
Authors: Münch, Guido
1959PASP...71..101M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: 4. High Temperature Subdwarfs with Anomalous Compositions
Authors: Munch, G.
1959LIACo...9...53M Altcode: 1959MSRSL...3...53M
No abstract at ADS
---------------------------------------------------------
Title: Internal Motions in the Orion Nebula
Authors: Münch, G.
1958RvMP...30.1035M Altcode: 1958IAUS....8.1035M
No abstract at ADS
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Title: Kinematics of the Filaments in the Crab Nebula
Authors: Münch, G.
1958RvMP...30.1042M Altcode: 1958IAUS....8.1042M
No abstract at ADS
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Title: Study of the Hydrogen and Helium II Lines in a High-Temperature
Subdwarf.
Authors: Münch, Guido
1958ApJ...127..642M Altcode:
The problem of line formation in a scheme of pure absorption is
considered For the case of a source function depending linearly on
mean optical depth, r, and a ratio, , of line to continuous absorption
coefficients independent of r, an approximate expression for the
line depth is derived similar in form to the Minnaert- interpolation
formula It is shown that this formula, for a given equivalent width,
underestimates the frequency-independent part of77 by a factor equal
to the central depth of the line, both for lines broadened by linear
Stark effect and for Doppler-broadened lines A procedure defining the
mean level of formation of the various parts of the contour of a line
with `7depending arbitrarily on r is developed. The representative
depths for the formation of a line as a whole, when it is broadened by
linear Stark effect, are also evaluated. The use of the theoretical
developments is illustrated by an analysis of the lines He ii x 4686
and H + He ii X 4340 observed in the spectrum of the 0-type subdwarf
HZ 44. Preliminary values of the electron pressure, p (r = 23),
the effective temperature, T , and the helium number abundance, Y,
are derived from the observed strength of X 4686, its ratio to 4340,
and the ionization equilibrium between the ions N Ir and N iii,
assuming = Constant. On the basis of the model log p, = 4.0, T, =
34000 K, and V = 0 28 thus obtained, the line intensities are again
calculated, allowing for the r-dependence of 77. The parameters p, and
T, of the zero approximation model atmosphere are found not to change
significantly on this account; but the value of V is reduced to V = 0.23
A surface gravity g = 10' 7 cm/sec2 and a visual absolute magnitude M,
= +37 if the mass were 1 0 and M = +12 if = 10 0, are estimated.
