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Interstellar Medium: more books (100)

Cosmic Dust: Dust, Molecule, Outer space, Interstellar medium, Nebula, Circumstellar disk, Planetary ring, Solar System, Zodiacal light, Asteroid belt, Kuiper belt, Stellar nucleosynthesis, Supernova
Physics &Chemistry of the Interstellar Medium 2006 publication by S.Kwok, 2006-01-01
The Luminiferous Ether: 1. Its Relation To The Electron And To A Universal Interstellar Medium; 2. Its Relation To The Atom (1919) by Frank W. Very, 2010-09-10
The Physics and Chemistry of the Interstellar Medium, 3rd Cologne-Zermatt Symposium, Abstract Book by Editor Volker Ossenkopf, 1998
Interstellar Media: Interstellar Cloud, Interstellar Medium, Interstellar Formaldehyde, Presolar Grains, Diffuse Interstellar Band, Superbubble
Astronomy and Planetary Science: The Stars and the Interstellar Medium Bk. 1 (Course S281) by Barrie William Jones, etc., et all 1994-12
The Luminiferous Ether. (I) Its Relation to the Electron and to a Universal Interstellar Medium; (II) Its Relation to the Atom by Frank W. Very, 1919
The Interstellar Medium by S.A.; Pikelner, S.B. Kaplan, 1970-01-01
Tetons 4; galactic structure, stars, and the interstellar medium; proceedings. ( by Stars and the Interstellar Medium (2 Conference on Tetons 4; Galactic Structure,
Structure and Dynamics of the Interstellar Medium: Proceedings of IAU Colloquium No. 120 Held on the Occasion of Guido's Jubilee in Granada, Spain, April 17-21, 1989 (Lecture Notes in Physics)
Star formation: Molecular Cloud, Plasma, Star, Astronomy, Interstellar Medium, Young Stellar Object, Binary Star, Initial Mass Function, Compact Star
Tetons 4; Galactic Structure, Stars, and the Interstellar Medium; Proceedings. by CharlesE.WoodwardEtAl, 2001
High Energy Astrophysics Volume 2 Stars, the Galaxy and the Interstellar Medium by Malcolm S. Longair, 1994
Interstellar medium

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The Heliosphere In The Local Interstellar Medium|KLUWER Academic Publishers
Books » The Heliosphere in the Local interstellar medium. The Heliospherein the Local interstellar medium. Add to cart. edited by
http://www.wkap.nl/prod/b/0-7923-4320-4

Extractions: This volume gives a comprehensive and integrated overview of current knowledge about the local interstellar medium (LISM) surrounding our heliosphere (HS). It is the result of the first workshop at ISSI, where both space physicists and astronomers presented and discussed their views on the density, velocity, temperature, composition, and morphology of the LISM and how it interacts with the HS. The volume is unique in its combination of data obtained by remote UV, EUV, and X-ray observations outside the HS with in situ observations of interstellar atoms, ions, and dust inside the HS. It thus demonstrates a new synergy between these two communities. The book is intended to provide active researchers in space physics and in astronomy with an up-to-date status report of its topic, and also to furnish the advanced graduate student with introductory material into the field. Kluwer Academic Publishers, Dordrecht
Cosmic Rays, Supernovae And The Interstellar Medium|KLUWER Academic Publishers
Books » Cosmic Rays, Supernovae and the interstellar medium. Cosmic Rays,Supernovae and the interstellar medium. Add to cart. Proceedings
http://www.wkap.nl/prod/b/0-7923-1278-3

Extractions: This book presents an introduction to an up-to-date review of the many interactions between the cosmic rays and the ISM. It includes introductory chapters on cosmic ray energetics, composition and propagation. The present stage of our knowledge of the gas, dust and clouds in the ISM is reviewed. Several chapters together present a thorough review of particle acceleration and of particle confinement and transport in the Galaxy. Gamma ray astronomy is treated in great detail.
Astronomy.com | CHIPS Will Dip Into The Interstellar Medium
CHIPS will Dip into the interstellar medium NASA s Cosmic Hot InterstellarPlasma Spectrometer (CHIPS) satellite will study space gases and dust.
http://www.astronomy.com/Content/Dynamic/Articles/000/000/001/168gslky.asp

Extractions: Despite what many of us were told, space is not a complete vacuum. There exists a thin interstellar medium composed of dust and gas, which holds the very beginning of stars. As extremely hot gas cools and breaks down, concentrations develop that become the seeds of these brilliant bodies. Yet the mystery of how the mixture of dust and gases transforms into stars remains. NASA scientists hope a new space probe will provide insight on the evolution of these building blocks of stars and planets.
Interstellar Medium
Links Science Astronomy interstellar medium. Reflection Nebulae(1). InterstellarMedium Web Search Results Below (Add Your Site or modify).
http://www.zookle.com/Science/Astronomy/Interstellar_Medium/
Interstellar Medium -- Britannica Concise Encyclopedia Online Article
Britannica Concise Encyclopedia, interstellar medium Britannica Concise. MLAstyle interstellar medium. Britannica Concise Encyclopedia. 2004.
http://concise.britannica.com/ebc/article?eu=393411
Interstellar Medium And The Milky Way
interstellar medium and the Milky Way. Full window version (looksa little nicer). Click Back interstellar medium (ISM). Though the
http://www.star.ucl.ac.uk/~idh/STROBEL/ismnotes/ismglxya.htm

Extractions: Our solar system is inside a large galaxy known as the Milky Way . All of the stars you can see at night and several hundred billion more are all bound together gravitationally into a huge cluster called a galaxy . Most of the stars in our galaxy are far enough away that we see them blended together in a thin band across our sky. If you are fortunate enough to view a dark sky outside of the glare of the city lights, you will see this milky band running through the constellations Cassiopeia, Perseus, Taurus, Monoceros, Vela, Crux, Norma, Sagittarius, Scutum, Aguila, Cygnus, and Lacerta. To people of long ago, this band looked like milk had been spilled along a pathway, so it was called the Milky Way. This chapter covers the radical discoveries made in the 20th century of the nature of the Milky Way and our place in it. Though the space between the stars is emptier than the best vacuums we have on Earth (those are enclosed spaces devoid of matter, not the household cleaning appliances), there is some material between the stars composed of gas and dust. This material is called the interstellar medium . The interstellar medium makes up between 10 to 15% of the visible mass of the Milky Way. About 99% of the material is gas and the rest is 'dust'. The interstellar medium affects starlight and stars (and planets) form from clouds in the interstellar medium, so it is worthy of study. Also, we can map out the structure of our Galaxy from measurements of the gas.
The Ionization Of The Local Interstellar Medium
The ionization of the local interstellar medium. While most of our workhas had the goal of understanding the structure and evolution
http://www.star.le.ac.uk/wd/ism.html

Extractions: While most of our work has had the goal of understanding the structure and evolution of white dwarfs, EUV observations of these stars can also tell us much about the intervening interstellar material. Although the original nebula from which the Solar System formed, about 4500 million years ago, will have been largely dissipated by the intense radiation from the young Sun and also left behind by the motion of the Solar System through interstellar space, more recent encounters with interstellar material may have affected us directly and at the very least influenced our astronomical observations. A Hammer-Aitoff plot in galactic coordinates, showing the distribution of white dwarf positions. The sizes of the symbols correspond to the HI column density along the line of sight. Squares = observations where a 228 Angstrom edge is not detected; triangles = 228 Angstrom edge detections analysed with H+He models; circles = 228 Angstrom edge detections analysed with heavy element models. The contours included indicate the distance (in pc) to the edge of the local cavity, as determined by Warwick et al. (MNRAS, Ionized material can be detected by the "shadowing" effect it has on the EUV spectra of other objects. Since, white dwarfs have strong EUV continua, they are ideal targets with which to search for interstellar absorption from HeI and HeII.
Galactic Interstellar Medium Dynamics And Cloud Formation
Galactic interstellar medium Dynamics and Cloud Formation. Giant molecularclouds and HI superclouds may be formed by largescale
http://www.astro.umd.edu/~ostriker/research/gal/project.html

Extractions: Giant molecular clouds and HI superclouds may be formed by large-scale gravitational instabilities in spiral/disk galaxies. Different types of instabilities may occur under varying galactic conditions. In the outer disks of galaxies (and away from spiral arms), shear tends to suppress the growth of the ordinary Jeans instability, but self-gravitational growth can occur via the swing amplifier mechanism (see movies below). Reduced shear and enhanced surface density within spiral arms make these regions more favorable for cloud formation and collapse. In arms and in inner disks where the rotation curve is closer to solid-body, Jeans-type instabilites can lead to growth as long as magnetic fields are present to transfer angular momentum out of growing condensations (see movies here ). Key observational support for the idea that gravitational instabilities determine the course of events comes from observed thresholds in surface density for active star formation in disks. Other evidence for the importance of self-gravitating instabilities is seen in M51, where prominent spurs jut out from the spiral arms at regular intervals, consistent with the predictions of our dynamical theory Using both semianalytic methods and time-dependent numerical simulations, our group is studying the development of self-gravitating clouds in the gaseous component of spiral galaxies. Our work has shown that nonlinear, nonaxisymmetric growth of structure in outer disks is indeed subject to threshold behavior, confirming the longstanding empirical model. We find that the critical values of the Toomre Q parameter for gravitational runaway are similar to observed star formation threshold values, and insensitive to the strength of the large-scale magnetic field. Our work has also shown how gravitational instabilities acting in galactic nuclei potentially leading to starbursts are qualitiatively quite different from outer-disk instabilities.
CITA Research 2001: Interstellar Medium
CITA Research September 2000 August 2001 interstellar medium. Studiesof the interstellar medium (ISM) address the diffuse gas
http://www.cita.utoronto.ca/webpages/AnnRep-2001/ResearchPages/ism.html

Extractions: Interstellar Medium Fiege , Matthews (McMaster) and Wilson (McMaster) have re-analyzed 850 micron SCUBA polarization data of OMC-3 region of the Orion A molecular cloud using improved software that was not available in 1998, when the data were taken. This region contains a bright filament that is partially fragmented into cores. Strong depolarization was observed toward the cores and along the spine of the filament. The polarization structure was modelled in detail using the technique outlined by Fiege and Pudritz (Ap.J, 2000, 544, 830), using their helical field model ( Fiege Fiege , Matthews and Moriarty-Schieven (JCMT) have used SCUBA polarimetry to map 3 star-forming systems of cores in Orion B. All 3 regions were found to contain polarization patterns that were indicative of highly ordered but non-uniform magnetic fields. Depolarization was found toward the bright cores in all 3 regions. NGC 2024 was the brightest and most interesting region mapped. 2 different models were proposed to account for the polarization data, and artificial polarization maps were computed for each model. Good agreement was found for a Fiege Using an 850 micron SCUBA map of the dark globule CB068 which contains a Class Young Stellar Object (YSO) and an associated bipolar outflow Fiege , Vallee (Herzberg) and Greaves (JCMT) have constructed a polarization model based on the Fiege The formation and collapse of a protostar involves the simultaneous infall and outflow of material in the presence of magnetic fields, self-gravity and rotation.
The Interstellar Medium
The interstellar medium. Studying the interstellar medium (ISM) within our ownGalaxy represents a considerable challenge, akin to understanding weather.
http://www.cita.utoronto.ca/webpages/CITA/annrep97/node23.html

Extractions: Next: Stars and Compact Objects Up: SCIENTIFIC OVERVIEW 1997 Previous: Galaxies Studying the Interstellar Medium (ISM) within our own Galaxy represents a considerable challenge, akin to understanding weather. Knowledge is required of non-linear feedback mechanisms for accumulating and dispersing the gaseous material and the energy budgets of the medium. Stars are born from cold dense condensations within giant molecular clouds, energetically heat and disrupt these birth environments and scatter the gas, release processed atoms and molecules back into the diffuse ISM, and eventually die, often releasing extensive outer stellar envelopes and sometimes producing supernova explosions. At CITA, active research on chemical processes in the ISM continues. Fundamental analysis of collision cross-sections between hydrogen molecules in ISM settings will aid in determining the rate of excitation of this most abundant molecule. Determination of the chemical enrichment of star - forming clouds from observations of spectral lines has resulted in constraints on the iron content within the Orion nebula. Computations of the collapse of magnetized cloud cores and the initial growth of stars produce a dynamic mass accumulation rate an order of magnitude larger than predicted by equilibrium theory. Magnetic fields in the Galaxy may also aid in the formation of dense star-formation sites based on models of the Parker instability, a process which funnels initially diffuse gas into small dense regions. Combining theory with multi-wavelength observations, is leading to insights on the modes of star formation and the environment surrounding star-formation sites.
Interstellar Medium - Wikipedia
PhatNav s Encyclopedia A Wikipedia . interstellar medium. See also Timelineof knowledge about the interstellar and intergalactic medium.
http://www.phatnav.com/wiki/wiki.phtml?title=Interstellar_medium
Topic: Stellar Systems; Interstellar Medium; Galactic And Extragalactic Objects
Geophysics, Astronomy, And Astrophysics , Stellar systems; interstellarmedium; galactic and extragalactic objects and systems; the Universe,.
http://topics.aip.org/98000_FS.html
Topic: Stellar Systems; Interstellar Medium; Galactic And Extragalactic Objects
Geophysics, Astronomy, And Astrophysics , Stellar systems; interstellar medium; galacticand extragalactic objects and systems; the Universe,.
http://topics.aip.org/98000.html

Extractions: Current Topic: Stellar systems; interstellar medium; galactic and extragalactic objects and systems; the Universe PACS Subject Classification Tree Geophysics, Astronomy, And Astrophysics Stellar systems; interstellar medium; galactic and extragalactic objects and systems; the Universe Warped product approach to universe with nonsmooth scale factor. Jaedong Choi and Soon-Tae Hong J. Math. Phys. (2) 642 (01 Feb 2004) Relativistic stars in differential rotation: bounds on the dragging rate and on the rotational energy. M. J. Pareja J. Math. Phys. (2) 677 (01 Feb 2004) Observational Constraints on Inflation. E. V. Mikheeva and V. N. Lukash Astron. Rep. (1) 2 (01 Jan 2004) Mixing of Metals during Stripping of Galactic Gaseous Halos. S. Yu. Dedikov and Yu. A. Shchekinov Astron. Rep. (1) 9 (01 Jan 2004) Massive Close Binary Stars and Gamma-ray Bursts. A. V. Tutukov and A. M. Cherepashchuk Astron. Rep. (1) 39 (01 Jan 2004) A. M. Gal'per and B. I. Luchkov Astron. Rep. (1) 35 (01 Jan 2004) Alfredo Herrera-Aguilar and Oleg V. Kechkin J. Math. Phys.
Infrared, Etc
There are also neutral gas atoms present which are destroyed close to the Sunbut are replenished from the interstellar medium. interstellar medium.
http://www.herts.ac.uk/astro_ub/aI_ub.html

Extractions: KEYWORD DEFINITIONS. - I - Infrared Electromagnetic radiation with a wavelength longer than visible light . The range is approximately between 10 and 10 metres. Infrared radiation is often observed from protostars and other objects which are deeply buried within dense interstellar clouds . Visible light is attenuated by these clouds but they can be penetrated by the longer wavelengths of infrared. Inflation . See inflationary cosmology. Inflationary cosmology . A revision to the standard model of the big bang to include an epoch when the universe was 10 seconds old during which the spacetime continuum expanded faster than the speed of light . As nothing was travelling through the spacetime continuum at a speed greater than that of light, no laws of physics are broken by this theory. The huge inflation of space was driven by the grand unified force separating into two: the strong nuclear force and the electroweak force . Tiny isotropic regions of the early universe were inflated to become larger than the observable universe. This aspect of the theory provides a satisfactory solution to the horizon problem . It also provides an answer to the flatness problem since by inflating the universe so much, any curvature becomes difficult to perceive. Hence as a result, the large scale geometry of the universe appears to be flat. This is in the same way as the surface of the Earth appears to us to be flat, even though we know it is really curved.
The Interstellar Medium
The interstellar medium. PHY410. ISM. Dyson, JE Williams, DA The Physics of theinterstellar medium Institute of Physics Publishing, (1997) ISBN 0-7503-0460-X.
http://www.ph.qmw.ac.uk/ughandbook/ism.shtml
Science Search > Interstellar Medium
Votes 2190. 3. interstellar medium Learning pages About ISM fromhistory of observation to current status of understanding. http
http://www.science-search.org/index/Astronomy/Interstellar_Medium/
INTERSTELLAR MEDIUM - Meaning And Definition Of The Word
interstellar medium Dictionary Entry and Meaning. WordNet Dictionary. Definitionn interstellar space including streams of protons moving from the stars.
http://www.hyperdictionary.com/dictionary/interstellar medium
Lecture 11: Interstellar Medium
interstellar medium. (1) The interstellar medium (that s just a fancy namefor the matter between stars) consists of lowdensity gas and dust.
http://www-astronomy.mps.ohio-state.edu/~ryden/ast162_3/notes11.html

Extractions: - Robert Frost The fact that we can look out far into the galaxy means that there must be very little matter between stars otherwise it would absorb all the starlight. Nevertheless, interstellar space is not entirely empty. 99% of the interstellar medium consists of very low density gas. How low in density is it? Let me tell you. The air we breathe has a density of approximately 10 molecules per cubic centimeter. (One cubic centimeter = 1 milliliter = 1/1000 liter). By contrast, the lowest density regions of interstellar space contains approximately 0.1 atoms per cubic centimeter.
The Interstellar Medium
The interstellar medium. COBE found the CII 158 m line to be the dominantcooling mechanism of the interstellar medium (Wright et al.
http://soral.as.arizona.edu/sofia2/node2.html

Extractions: Next: Protostellar Collapse and Disk Up: Scientific Motivation Previous: Scientific Motivation The proposed system will be capable of performing high spectral resolution studies of a number of important atomic and molecular species, including [SiI], [OI], [CII], CO, CH, OH, and [NII]. Of particular interest are the [CII] 158 m and [NII] 205 m lines, and a variety of lines from simple hydrides such as OH, CH, and CH COBE found the [CII] 158 m line to be the dominant cooling mechanism of the interstellar medium (Wright et al. 1991; Bennet et al. et al. 1993; Stutzki et al. et al. times more sensitive per pixel and have 16 times the spatial coverage of earlier heterodyne instruments flown on the KAO. The potential power of STAR in probing conditions in and around molecular clouds is illustrated in Figure 1. In the middle of the figure we show an image of NGC 6334 made in CO J=4 from AST/RO with a receiver system constructed in the PI's lab. The small square of emission in the top right hand corner is the size of the region that could be mapped in CII at full beam spacings with a single receiver channel in one flight ( hrs). The second square shows the region that could be mapped with STAR in the same period of time, essentially the whole cloud. The CII spectra at the bottom left were taken by Borieko and Betz (1995). The width and complexity of the line profiles are well matched to the 40 km/s velocity coverage and 0.125 km/s velocity resolution available in each STAR pixel.
The Interstellar Medium
observations. The interstellar medium. Several groups work on problemsrelated to the interstellar matter and its distribution and physics.
http://www.astro.su.se/aar9798/node18.html

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