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Добірка наукової літератури з теми "Interstellar matter"

Автор: Grafiati

Опубліковано: 4 червня 2021

Оновлено: 29 липня 2024

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Статті в журналах з теми "Interstellar matter"

1

Lequeux, J., J. S. Mathis, K. S. de Boer, S. D’Odorico, B. G. Elmegreen, D. Flower, H. Habing, et al. "34. Interstellar Matter (Matiere Interstellaire)." Transactions of the International Astronomical Union 20, no. 01 (1988): 423–71. http://dx.doi.org/10.1017/s0251107x0000732x.

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Анотація:

The previous report started with optimistic remarks about the increasing importance of the study of interstellar matter in astronomy. This trend has largely been confirmed in the 1985-87 period and it is clear that the subject of our Commission is one of the most active fields of astronomical research. This is also shown by the rapidly growing number of members and by the constitution of new working groups. The major new event in the period has undoubtly been the availability of IRAS data.

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2

Habing, H. J., E. Falgarone, D. Flower, P. G. Martin, M. R. Rosa, T. Lozinskaya, and M. Dopita. "34 Interstellar Matter: Matiere Interstellaire." Transactions of the International Astronomical Union 22, no. 1 (1994): 367–97. http://dx.doi.org/10.1017/s0251107x00008117.

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3

Dopita, Michael A., Rafael Bachiller, Michael Burton, John Dyson, Debra Elmegreen, Thomas Henning, Sun Kwok, et al. "Division VI: Interstellar Matter: (Matière Interstellaire)." Transactions of the International Astronomical Union 24, no. 1 (2000): 277–80. http://dx.doi.org/10.1017/s0251107x00003175.

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Анотація:

Division VI of the International Astronomical Union deals with Interstellar Matter, and incorporates Commission 34. It gathers astronomers studying the diffuse matter in space between the stars, ranging from primordial intergalactic clouds via dust and neutral and ionised gas in galaxies to the densest molecular clouds and the processes by which stars are formed. There are approximately 730 members. The working groups in Planetary Nebulae and Cosmochemistry have served us well in organising periodic seminars in these subject areas. However, the Organising Committee has recognised that other developing areas of the ISM are not properly represented in the current organisation. In January 1997, the Division formed a new ISM working group on Star Forming Regions including cross-divisional representation to monitor progress in their fields and to help develop proposals for future IAU Symposia or Colloquia. In the future, especially in view of the rapid developments in spaceborne X-ray and IR astronomy, Division VI also hopes to form other working groups on the Hot ISM and the Extragalactic ISM.

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4

Reipurth, Bo. "Division VI: Interstellar Matter (Matiere Interstellaire)." Transactions of the International Astronomical Union 25, no. 2 (2007): 157–58. http://dx.doi.org/10.1017/s0251107x00026729.

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5

Reipurth, Bo, Rafael Bachiller, John Dyson, José Franco, Thomas Henning, Trung Hua, Sun Kwok, et al. "Division VI: Interstellar Matter: (Matiere Interstellaire)." Transactions of the International Astronomical Union 25, no. 1 (2002): 283–86. http://dx.doi.org/10.1017/s0251107x00001577.

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6

Bochkarev, Nikolai G. "Local interstellar matter and interstellar bubbles." Astronomical & Astrophysical Transactions 3, no. 1 (November 1992): 3–16. http://dx.doi.org/10.1080/10556799208230534.

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7

Peimbert, M., J. Lequeux, S. D’Odorico, B. G. Elmegreen, E. B. Kostyakova, J. S. Mathis, U. Mebold, et al. "34. Interstellar Matter." Transactions of the International Astronomical Union 19, no. 1 (1985): 437–78. http://dx.doi.org/10.1017/s0251107x00006532.

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Анотація:

It has become more evident during the last three years that the study of interstellar matter is paramount to understand the evolution of the universe and its constituents. From observations of the present state of the interstellar medium, in our galaxy, in other galaxies, and between galaxies, it is possible to test theories of: evolution of the universe, formation and evolution of galaxies, formation and evolution of stars and of the evolution of the interstellar medium itself. The amount of information on the interstellar medium that has been gathered during the 1982-1984 period has been very large and the theoretical models that have been ellaborated to explain these observations have been very numerous, these facts show that the subject of our Commission constitutes a very active field of astronomical research.

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8

Dyson, John, Thomas J. Millar, Bo Reipurth, You-Hua Chu, Gary J. Ferland, José Franco, Chon Trung Hua, et al. "DIVISION VI: INTERSTELLAR MATTER." Proceedings of the International Astronomical Union 3, T26B (December 2007): 173. http://dx.doi.org/10.1017/s1743921308023971.

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Анотація:

Division VI gathers astronomers studying the diffuse matter in space between stars, ranging from primordial intergalactic clouds, via dust and neutral and ionized gas in galaxies, to the densest molecular clouds and the processes by which stars are formed.

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9

Millar, Thomas J., You Hua Chu, John E. Dyson, Dieter Breitschwerdt, Michael G. Burton, Sylvie Cabrit, Paola Caselli, et al. "DIVISION VI: INTERSTELLAR MATTER." Proceedings of the International Astronomical Union 4, T27A (December 2008): 267–72. http://dx.doi.org/10.1017/s1743921308025659.

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10

Dyson, John, Tom Millar, You-Hua Chu, Gary Ferland, Pepe Franco, Trung Hua, Susana Lizano, et al. "Division VI: Interstellar Matter." Proceedings of the International Astronomical Union 1, T26A (December 2005): 267–71. http://dx.doi.org/10.1017/s1743921306004662.

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Анотація:

Commission 34 covers diffuse matter in space on scales ranging from the circumstellar to the galactic and intergalactic. As such it has enormous scope and because of this, it alone forms Division VI. Key aspects include star formation, matter around evolved stars, astrochemistry, nebulae, galactic and intergalactic clouds and the multitude of effects of the interaction of stars with their surroundings. Associated with these areas are a huge range of physical and chemical processes including hydrodynamics and magnetohydrodynamics, radiative processes, molecular physics and chemistry, plasma processes and others too numerous to name. These are complemented by an equally huge range of observational studies using practically all space and ground-based instrumentation at nearly all observable wavelengths. A glance at any data-base of publications over the past few years attests to the vigorous state of these studies. The current membership of the Division is around 800. It also has three separate working groups.

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Дисертації з теми "Interstellar matter"

1

Hopwood, Madelaine E. L. "Interstellar matter in globular clusters." Thesis, Keele University, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.323681.

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2

Danforth, Charles Weston. "Interstellar matter kinematics in the magellanic clouds." Available to US Hopkins community, 2003. http://wwwlib.umi.com/dissertations/dlnow/3080648.

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3

Hurst, Mark Edward. "Observational studies of stellar, circumstellar and interstellar matter." Thesis, University of Nottingham, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.312198.

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4

Kristen, Helmuth. "Dynamics of the interstellar matter in galaxies : isolated barred spiral galaxies : cloud formation processes /." Stockholm : Univ, 1998. http://bvbr.bib-bvb.de:8991/F?func=service&doc_library=BVB01&doc_number=008210174&line_number=0001&func_code=DB_RECORDS&service_type=MEDIA.

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5

Malawi, Abdulrahman Ali. "Atomic hydrogen associated with high latitude IRAS cirrus clouds." Thesis, University of Manchester, 1989. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.664465.

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6

Roser, Joseph E. Vidali Gianfranco. "Laboratory simulations of chemical reactions on dust grains in the interstellar medium." Related electronic resource: Current Research at SU : database of SU dissertations, recent titles available full text, 2004. http://wwwlib.umi.com/cr/syr/main.

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7

Smith, Keith T. "Studies of interstellar matter on scales from 10AU to 10 kpc." Thesis, University of Nottingham, 2010. http://eprints.nottingham.ac.uk/12504/.

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Анотація:

This thesis presents four optical spectroscopic studies of absorption by matter in the diffuse interstellar medium on scales ranging from 10 AU to 10 kpc. The observations investigate two current problems in interstellar medium (ISM) research: small-scale structure (SSS), and the diffuse interstellar bands (DIBs). Very high spectral resolution observations of interstellar Na I, Ca I, Ca II, K I and CH absorption towards kappa Vel are presented. Combined with observations over the last 15 years taken from the literature, the small-scale structure in front of this star is probed on scales of ~ 10 AU. The high resolution and signal-to-noise of the new observations allow detailed modelling of the absorption profiles and the identification of multiple absorption components. For the two narrowest components, the line profile models are used to constrain the temperature, depletion, electron density and total number density within the structures. Diffuse interstellar bands are used as probes of SSS in long-slit observations of lines-of-sight towards three binary/multiple star systems: HD 168075/6, HD 176269/70 and four members of the mu Sgr system, one of which is identified as a member for the first time. The results show clear variations in DIB absorption in the HD 168075/6 and mu Sgr systems over scales of ~ 50,000-200,000 AU, and demonstrate the efficacy of medium-resolution observations of DIBs for identification of small-scale structure in the ISM. Multi-object spectroscopy of 452 stars in the omega Cen globular cluster is also presented, which probes interstellar absorption by Na I, Ca II and DIBs in two dimensions, on scales of ~ 1 pc. The first detections of diffuse interstellar bands in the M33 galaxy are reported. Multi-object spectroscopy of 43 stars is used to derive spectral types and reddenings, and measure DIB absorption across the disk of the galaxy (~ 10 kpc). Very strong DIB absorption per unit E(B-V) is found for one star in the sample, towards which a total of seven DIBs are detected.

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8

van, Dishoeck E. F. "Interstellar C2, CH, and CN in Translucent Molecular Clouds." Steward Observatory, The University of Arizona (Tucson, Arizona), 1988. http://hdl.handle.net/10150/623918.

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Анотація:

Optical absorption line techniques have been applied to the study of a number of translucent molecular clouds in which the total column densities are large enough that substantial molecular abundances can be maintained. Results are presented for a survey of absorption lines of interstellar C2, CH, and CN. Detections of CN through the A2II -X2E+ (1,0) and (2,0) bands of the red system are reported, and are compared with observations of the blue system for one line of sight. The population distributions in C2 provide diagnostic information on temperature and density. The measured column densities of the three species can be used to test details of the theory of molecule formation in clouds where photo -processes still play a significant role. The C2 and CH column densities are strongly correlated with each other and probably also with the H2 column density. In contrast, the CN column densities are found to vary greatly from cloud to cloud. The observations are discussed with reference to detailed theoretical models.

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9

Walker, Constance Elaine. "A submillimeter-millimeterwave study of the molecular gas in the nuclear regions of three nearby starburst galaxies." Diss., The University of Arizona, 1991. http://hdl.handle.net/10150/185738.

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In this thesis we use multi-transitional millimeter/submillimeter-wave molecular spectroscopy of CO and CS to determine the state of the molecular gas in the central regions of three starbursts: M82, IC342, and M83. High angular resolution 60 and 100 μm IRAS images provide complementary information about the thermal dust emission in IC342 and M83. Our CO observations reveal the presence of a molecular ring and supernovae driven wind in M82. In IC342 and M83 there is evidence for molecular bars and central rotating cores. The CO and CS line ratio analyses suggest a multicomponenet medium with clouds externally heated by ultraviolet flux from young, massive stars. Excitation temperatures typically range from 20 to 40 K throughout the nuclear regions of the sample galaxies. In M82 the CO and CS optical depths are ∼ 1. Our analysis of ¹²CO indicates that this gas is optically thick toward the centers of IC342 and M83. The molecular gas mass in each galaxy is ∼ 5x10⁷ M(⊙). We derive an average cloud size between 0.1 and 1 pc in the nuclear region of M82 and M83. An average cloud size of 10 pc is found over a comparable region in IC342. From tidal arguments we find that the clouds must have densities greater than 100 to 1000 cm⁻³ to survive. If the clouds are virialized, then the expected individual cloud linewidths are 9, 40, 5 and 27 km/s for M82, IC342, M83 and the Milky Way, respectively. For the clouds to be pressure-bound, inter-cloud pressures > 10x the peak value in the Galactic Center are required. If the magnetic fields are frozen into the gas, an average field strength of 8.5 mG is needed to support the nuclear clouds in each galaxy from collapse. Enhanced IRAS images reveal bright, compact nuclear components in IC342 and M83. HII regions are seen along spiral arms in IC342 and a dusty bar is seen in M83. The similarity between radio continuum maps and the high resolution IRAS maps suggest that infrared emission arises from HII regions. Using an emissivity law of β ∼ 1.5, the derived dust temperatures in the nuclei of IC342 and M83 are essentially the same as the gas excitation temperatures. For this to occur, gas densities of > 10⁴ cm⁻³ are implied. We derive a star-formation efficiency, ∊, of 77, 60, 10 and 2% for M82, M83, IC342, and the Milky Way, respectively. We find evidence that the gas surface density toward the centers of these galaxies is α ∊. We estimate star-formation rates of 16, 6, 2.5, and .06 M(⊙)/yr for M82, M83, IC342 and the Milky Way. The gas depletion timescales are a few million years for M82 and M83 and a few times 10⁷ and 10⁸ years in IC342 and the Milky Way. We find a strong correlation between cloud diameter and star-formation efficiency, with smaller clouds found in galaxies with higher ∊. We conclude these smaller clouds are a by-product and not a causal factor of the starburst phenomenon.

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10

Porayko, Nataliya Konstantinovna [Verfasser]. "Probing the Interstellar Medium and Dark Matter with Pulsars / Nataliya Konstantinovna Porayko." Bonn : Universitäts- und Landesbibliothek Bonn, 2020. http://d-nb.info/1207923710/34.

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Книги з теми "Interstellar matter"

1

Spitzer, Lyman. Physical processes in the interstellar medium. New York: Wiley, 1998.

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2

Voigt, H. H., ed. Interstellar Matter, Galaxy, Universe. Berlin/Heidelberg: Springer-Verlag, 1999. http://dx.doi.org/10.1007/b46102.

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3

1936-, Winnewisser G. (Gisbert), and SpringerLink (Online service), eds. Interstellar Molecules: Their Laboratory and Interstellar Habitat. Berlin, Heidelberg: Springer-Verlag Berlin Heidelberg, 2011.

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4

David, Skillman Evan, and University of Minnesota, eds. The Minnesota lectures on extragalactic neutral hydrogen: A series of lectures presented at the University of Minnesota, Minneapolis, Minnesota, from 27 March 1994 [i.e. 1995] to 2 June 1994 [i.e. 1995]. San Francisco, Calif: Astronomical Society of the Pacific, 1996.

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5

1974-, Haverkorn M., and Goss W. M, eds. SINS--small ionized and neutral structures in the diffuse interstellar medium: Proceedings of a workshop held at the National Radio Astronomy Observatory, Socorro, New Mexico, USA, 21-24 May 2006. San Francisco: Astronomical Society of the Pacific, 2007.

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6

McComas, David J. Interstellar Boundary Explorer (IBEX). Dordrecht: Springer, 2010.

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7

Kim, Dong-Woo, and Silvia Pellegrini, eds. Hot Interstellar Matter in Elliptical Galaxies. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-0580-1.

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8

International Astronomical Union. General Assembly, ed. Hot interstellar matter in elliptical galaxies. Heidelberg: Springer, 2011.

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9

Meeting, Royal Society (Great Britain) Discussion. Material content of the universe: Proceedings of a Royal Society Discussion Meeting held on 23 and 24 October 1985. London: Royal Society, 1987.

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10

1944-, Ikeuchi S., and United States. National Aeronautics and Space Administration., eds. The disk-halo connection and the nature of the interstellar medium. Baltimore, MD: Space Telescope Science Institute, 1990.

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Частини книг з теми "Interstellar matter"

1

Flower, D. R., M. A. Dopita, F. C. Bruhweiler, M. G. Burton, D. M. Elmegreen, E. Falgarone, T. A. Lozinskaya, et al. "Interstellar Matter Matiere Interstellaire." In Reports on Astronomy, 397–414. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5762-9_33.

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2

McNally, Derek. "Interstellar Matter (Matiere Interstellaire)." In Reports on Astronomy, 373–420. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3364-7_24.

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3

Lequeux, J., J. S. Mathis, K. S. de Boer, S. D’Odorico, B. G. Elmegreen, D. Flower, H. Habing, et al. "Interstellar Matter." In Reports on Astronomy, 423–71. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2981-4_25.

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4

Habing, H. J., E. Falgarone, D. Flower, M. R. Rosa, T. Lozinskaya, and M. Dopita. "Interstellar Matter." In Reports on Astronomy, 367–97. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1100-3_25.

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5

West, Richard M. "Interstellar Matter." In Reports on Astronomy, 437–78. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5392-5_25.

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6

Sofue, Yoshiaki. "Interstellar Matter." In Galactic Radio Astronomy, 33–56. Singapore: Springer Singapore, 2017. http://dx.doi.org/10.1007/978-981-10-3445-9_2.

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7

Hanslmeier, Arnold. "Interstellar Matter." In Introduction to Astronomy and Astrophysics, 463–78. Berlin, Heidelberg: Springer Berlin Heidelberg, 2022. http://dx.doi.org/10.1007/978-3-662-64637-3_12.

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8

Verschuur, Gerrit L. "An Extraterrestrial Matter." In Interstellar Matters, 290–302. New York, NY: Springer New York, 1989. http://dx.doi.org/10.1007/978-1-4612-4522-3_24.

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9

Verschuur, Gerrit L. "Molecules and Interstellar Matter." In Interstellar Matters, 234–47. New York, NY: Springer New York, 1989. http://dx.doi.org/10.1007/978-1-4612-4522-3_20.

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10

Verschuur, Gerrit L. "A Mysterious Interstellar Matter." In Interstellar Matters, 280–89. New York, NY: Springer New York, 1989. http://dx.doi.org/10.1007/978-1-4612-4522-3_23.

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Тези доповідей конференцій з теми "Interstellar matter"

1

Blades, J. C., and N. Panagia. "Interstellar abundances towards SN1987A." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.38015.

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2

Hovestadt, Dietrich, and Eberhard Möbius. "Interstellar neutrals in interplanetary space." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.38004.

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3

Meyer, Jean-Paul. "Elemental abundances in the interstellar medium ... and elsewhere." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.37991.

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4

Sahu, Kailash C., S. R. Pottasch, and Meenakshi Sahu. "Primordial lithium abundance from interstellar lithium lines towards SN 1987A." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.37984.

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5

Iacob, F. "ELECTRON-MOLECULAR CATION COLLISIONS IN INTERSTELLAR SPACE." In VI Conference on Active Galactic Nuclei and ravitational Lensing. Astronomical Observatory Belgrade, Volgina 7, 11060 Belgrade 38, Serbia, 2024. http://dx.doi.org/10.69646/aob24007.

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Анотація:

In the interstellar medium, highly excited states of molecules can form a state of matter called Rydberg Matter. Mainly, they are formed by the promotion of an electron from the lower layers of the molecule to the highly excited ones. However, these can also be formed by temporarily capturing an electron in high energy orbitals following its collisions with cations. This paper focuses on the latter, the collisional approach, which is more suitable for explaining these highly excited states that can be found in this environment. It should be mentioned that in this environment cations are abundant and the probability of collision with electrons is high generating with high rates these highly excited states of the neutral called Rydberg states. It is found that low-energy electrons, such as those in the interstellar medium, generate these neutral capture states much more frequently. These results provide a quantitative description of Rydberg matter, which by its properties is a good candidate for dark matter. As a case study the molecular cation NS+ is considered as a target for obtaining strongly excited states of neutral NS after collisions with low energy electrons.

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6

Moniez, Marc. "Searching for Galactic Hidden Gas through interstellar scintillation: The OSER project." In Identification of dark matter 2008. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.064.0097.

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7

Green, James C., Patrick Jelinsky, and Stuart Bowyer. "The ratio of neutral helium to neutral hydrogen in the local interstellar medium." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.37979.

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8

Kajino, Fumiyoshi, Shinsuke Abe, Mizuho Arahori, Dario Barghini, Mario Edoardo Bertaina, Marco Casolino, Alberto Cellino, et al. "DIMS Experiment for Dark Matter and Interstellar Meteoroid Study." In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0554.

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9

Soutoul, A., and P. Ferrando. "Propagation of cosmic-rays nuclei in the interstellar medium: The importance of energy losses revisited." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.37975.

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Kajino, Fumiyoshi. "DIMS Experiment for Macroscopic Dark Matter and Interstellar Meteoroid Study." In 38th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2023. http://dx.doi.org/10.22323/1.444.1376.

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Звіти організацій з теми "Interstellar matter"

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Wells, James D. Illuminating dark matter and primordial black holes with an interstellar antiproton spectrometer. Office of Scientific and Technical Information (OSTI), November 1998. http://dx.doi.org/10.2172/9903.

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