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Molecular abundances in the Sagittarius A molecular cloud.

We have obtained column densities for HCO+, HCO, HCS+, C3H2, HC5N, SiO, OCS, HCOOH, CH3CH2OH, and CH3CCH toward Sgr A. The fractional abundance of SiO relative to molecular hydrogen in Sgr A is comparable to that for the Orion plateau, approximately 10(-7)-10(-8), which may be a typical value for hot clouds. The abundances of HCO, CH3CH2OH and CH3CCH all appear to be enhanced relative to other molecular clouds such as Sgr B2.

Astronomical Phenomena↗

Crystallization of amorphous ice as the cause of comet P/Halley's outburst at 14 AU.

The post-perihelion eruption of comet P/Halley, detected in Feb. 1991 and believed to have started 3 months earlier, can be explained by crystallization of amorphous ice taking place in the interior of the porous nucleus, at depths a few tens of meters, accompanied by the release of trapped gases. Numerical calculations show that for a bulk density of 0.5 g cm-3 and a pore size of 1 millimicron crystallization occurs on the outbound leg of comet P/Halley's orbit, at heliocentric distances between 5 AU and 17 AU. The trapped gas is released and flows to the surface through the porous medium. It may also open wider channels, as the internal pressures obtained surpass the tensile strength of cometary ice. The outflowing gas carries with it grains of ice and dust, and thus can explain the large amounts of dust observed in the coma at 14.3 AU and beyond. The typical decline time of the process is found to be on the order of months, in agreement with observations. The rate of outgassing is two or three orders of magnitude higher than in quiescence. In an asymmetric, non-uniform nucleus--in contrast to the one-dimensional spherical model--the process should occur intermittently, such as was observed for comet P/Halley beyond 5 AU.

Astronomical Phenomena↗

H2CS abundances and ortho-to-para ratios in interstellar clouds.

Several H2CS ortho and para transitions have been observed toward interstellar molecular clouds, including cold, dark clouds and star-forming regions. We derive H2CS fractional abundances f(H2CS) approximately 1-2 10(-9) relative to molecular hydrogen towards TMC-1, Orion A, and NGC 7538, and approximately 5 10(-10) for L134N. The H2CS ortho-to-para ratios in TMC-1 are approximately 1.8 towards the cyanopolyyne peak and the ammonia peak, which may indicate the thermalization of H2CS on 10 K grains. We derive a ratio of approximately 3, the statistical value, for Orion (3N, 1E) and NGC 7538, while we find a value approximately 2 for Orion (KL).

Astronomical Phenomena↗

Abundance and chemistry of interstellar HOCO+.

We derive HOCO+ column densities approximately 10(15) cm-2 toward the Galactic center and < or = 10(12) cm-2 for cold dark clouds from observations and an LVG model. We mapped the HOCO+ 4(04)-3(03) line toward Sgr A. The fractional abundance of HOCO+ in the Galactic center region is three orders of magnitude larger than predicted by quiescent ion-molecule chemistry and an order of magnitude larger than predicted by a MHD shock model. If HOCO+ traces interstellar CO2, the implied high abundance ([CO2] approximately [CO]) in the Galactic center may result from UV photolysis of grain mantles.

Astronomical Phenomena↗

HCl absorption toward Sagittarius B2.

We have detected the 626 GHz J = 1 --> 0 transition of hydrogen chloride (H35Cl) in absorption against the dust continuum emission of the molecular cloud Sagittarius B2. The observed line shape is consistent with the blending of the three hyperfine components of this transition by the velocity profile of Sgr B2 observed in other species. The apparent optical depth of the line is tau approximately 1, and the minimum HCl column density is 1.6 x 10(14) cm-2. A detailed radiative transfer model was constructed which includes collisional and radiative excitation, absorption and emission by dust, and the radial variation of temperature and density. Good agreement between the model and the data is obtained for HCl/H2 approximately 1.1 x 10(-9). Comparison of this result to chemical models indicates that the depletion factor of gas-phase chlorine is between 50-180 in the molecular envelope surrounding the SgrB2(N) and (M) dust cores.

Astronomical Phenomena↗

Infrared emission from comets.

A brief discussion of the infrared observations from 4 to 20 micrometers of seven comets is presented. The observed infrared emission from comets depends primarily on their heliocentric distance. A model based on grain populations composed of a mixture of silicate and amorphous carbon particles in the mass ratio of about 40 to 1, with a power-law size distribution similar to that inferred for comet Halley, is applied to the observations. The model provides a good match to the observed heliocentric variation of both the 10 micrometers feature and the overall thermal emission from comets West and Halley. Matches to the observations of comet IRAS-Araki-Alcock and the antitail of comet Kohoutek require slightly larger grains. While the model does not match the exact profile and position of the 3.4 micrometers feature discovered in comet Halley, it does produce a qualitative fit to the observed variation of the feature's strength as a function of heliocentric distance. The calculations predict that the continuum under the 3.4 micrometers feature is due primarily to thermal emission from the comet dust when the comet is close to the Sun and to scattered solar radiation at large heliocentric distances, as is observed. A brief discussion of the determination of cometary grain temperatures from the observed infrared emission is presented. It is found that the observed shape of the emission curve from about 4 to 8 micrometers provides the best spectral region for estimating the cometary grain temperature distribution.

Astronomical Phenomena↗

Life in the universe

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Astronomical Phenomena↗

Life's origin: the cosmic, planetary and biological processes.

From elements formed in interstellar furnaces to humans peering back at the stars, the evolution of life has been a long, intricate and perhaps inevitable process. Life as we know it requires a planet orbiting a star at just the right distance so that water can exist in liquid form. It needs a rich supply of chemicals and energy sources. On Earth, the combination of chemistry and energy generated molecules that evolved ways of replicating themselves and of passing information from one generation to the next. Thus, the thread of life began. This chart traces the thread, maintained by DNA molecules for much of its history, as it weaves its way through the primitive oceans, gaining strength and diversity along the way. Organisms eventually moved onto the land, where advanced forms, including humans, ultimately arose. Finally, assisted by a technology of its own making, life has reached back out into space to understand its own origins, to expand into new realms, and to seek other living threads in the cosmos.

Animals↗

Impact process: an important geological phenomenon.

The impact process was for a long period of time, even after a wider acceptance among the geological community, considered to be a marginal phenomenon in the Earth sciences. The first decade or two have showed an importance of the process itself and consequent events only too clearly. The present paper is a review describing the history and development of the impact hypothesis, structure and origin of impact craters, influence of huge impacts on the living environment and other aspects of the impact process from the point of view of geology s.l.

Animals↗

The search for extraterrrestrial life: recent developments. A report on IAU Symposium 112.

This paper is a report on the International Symposium "The Search for Extraterrestrial Life: Recent Developments" which was held in Boston, Massachusetts, USA, 18-21 June 1984. It was the first IAU Symposium organised by Commission 51 of the International Astronomical Union (IAU), and was co-sponsored by the IAF/IAA, COSPAR, ISSOL and IUBS. This report describes the highlights from the seven Sessions and two special events of the Symposium, which was attended by 145 participants from 18 countries and in which more than 50 invited and contributed papers were presented. It also discusses the future plans and activities of IAU Commission 51.

Astronomy↗

[Macroscopic fluctuations of discrete distribution forms as a consequence of the arithmetic and cosmophysical causes].

The recent investigations are reviewed of the "macsroscopic fluctuations", i.e. synchronous on local time changes in probability of the appearance of the same detailed structure of distribution (histograms) of the rates of different processes, at the same or at different geographic points. Gravitation nonhomogeneousity is considered as a probable cause of these phenomena.

Earth, Planet↗