61. 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

Title Authors Affiliation ISBN ISSN advanced search search tips Books The Heliosphere in the Local Interstellar Medium The Heliosphere in the Local Interstellar Medium Add to cart edited by Rudolf von Steiger International Space Science Institute, Bern, Switzerland R. Lallement M.A. Lee University of New Hampshire, Durham, USA Book Series: SPACE SCIENCES SERIES OF ISSI Volume 1 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

62. 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

Title Authors Affiliation ISBN ISSN advanced search search tips Books Cosmic Rays, Supernovae and the Interstellar Medium Cosmic Rays, Supernovae and the Interstellar Medium Add to cart Proceedings of the NATO Advanced Study Institute, Erice, Italy, July 26-August 5, 1990 edited by Maurice M. Shapiro Dept. of Physics and Astronomy, University of Maryland, College Park, USA Rein Silberberg Universities Space Research Association, Washington, DC, USA John P. Wefel Dept. of Physics and Astronomy, Louisiana State University, Baton Rouge, USA Book Series: NATO SCIENCE SERIES: C: Mathematical and Physical Sciences (continued within NATO SCIENCE SERIES II: Mathematics, Physics and Chemistry Volume 337 Galactic cosmic rays have far-reaching effects on the interstellar medium (ISM) and they are, in turn, profoundly affected by the particles and fields in space. Supernova remnants and their expanding shock fronts pervade the Galaxy, heating the interstellar medium and accelerating the cosmic rays. 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. The volume is of interest to all astrophysicists and scientists in related disciplines.

63. 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

OUR SOLAR SYSTEM OTHER SOLAR SYSTEMS STARS GALAXIES ... Vendor Directory = registered content Articles Photo Gallery Events Organizations Vendor Directory Register to become a member! Gain access to our customizable Star Chart, Forums, Astronomy Quiz, Weekly Newsletter, and more. Register to become a member Learn More Help with login/registration Forgot your Password? Member Login Username Password SCIENCE NEWS SPACE MISSIONS CHIPS will Dip into the Interstellar Medium NASA's Cosmic Hot Interstellar Plasma Spectrometer (CHIPS) satellite will study space gases and dust. by Jeremy McGovern While orbiting Earth, the CHIPS satellite will study the very hot, very low-density gas in the vast spaces between the stars in our astronomical neighborhood. NASA 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. Scheduled for launch at 7:45 p.m. EST on January 11, the Cosmic Hot

64. 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/

zOO KLE link exchange top 100 Add Your Site Jokes ... Wallpaper Links: Science: Astronomy: Interstellar Medium Home Science Astronomy : Interstellar Medium Subcategories: Emission Nebulae Planetary Nebulae Reflection Nebulae Interstellar Medium Web Search Results Below Add Your Site or modify Colorado Model of the Local Interstellar Cloud The hydrogen cloud in which the Solar System is immersed. 3D pictures of the cloud, view from any direction, movie, calculate hydrogen column density in any direction. http://casa.colorado.edu/~sredfiel/ColoradoLIC.html Interstellar Medium Learning pages About ISM from history of observation to current status of understanding. http://www-ssg.sr.unh.edu/tof/Outreach/Interstellar/ Interstellar Molecules evolutionary cycle Evolutionary cycle of Interstellar Organic Molecules - Fullerenes, PAHs, Polyyenes, and biomolecules. http://www.shantanurastogi.homestead.com/files/ismol.html Nebulae Part of a larger site on plasma physics. http://fusedweb.pppl.gov/CPEP/Chart_Pages/5.Plasmas/Nebula.html Observations of Interstellar Molecules About observation of Interstellar molecules in the ISM and Physical information obtained from them.

65. 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

66. 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

Interstellar Medium and the Milky Way Full window version 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. Interstellar Medium (ISM) 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.

67. 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

The ionization of the local interstellar medium 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.

68. 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

Galactic Interstellar Medium Dynamics and Cloud Formation 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.

69. 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

CITA Research September 2000 - August 2001 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.

70. 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

Next: Stars and Compact Objects Up: SCIENTIFIC OVERVIEW 1997 Previous: Galaxies The Interstellar Medium 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.

71. 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

72. 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 and systems; the Universe Topics: Geophysics, Astronomy, And Astrophysics , Stellar systems; interstellar medium; galactic and extragalactic objects and systems; the Universe

73. 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

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.

74. 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

Astronomy 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.

75. 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

The Interstellar Medium PHY-410 ISM RUNS EVERY SECOND YEAR NOT GIVEN 2003/2004 This course has a HOME PAGE which gives further details for current students Year 2/3 Semester 3 or 5 Level 2/3 1 course unit Timetable Block C,E,G Lectures: 24, 43, 45 Course Organiser: Deputy: Prerequisites: PHY-212 Examination: Lectures: Practical work: none Ancillary teaching: weekly exercises Synopsis: SYLLABUS STRUCTURE OF THE ISM Molecular clouds, interstellar dust, atomic and ionised gas. STRUCTURE AND EVOLUTION OF MOLECULAR CLOUDS Thermal and dynamical stability of clouds, cloud collapse, fragmentation, rotation. IONISED GAS IN THE ISM Nebulae, ions in dark clouds. MOLECULAR AND ATOMIC LINES Excitation and thermodynamics, use as diagnostics of the ISM. CHEMISTRY IN THE ISM Molecular and atomic make-up of the ISM, interstellar chemical processes. INTERSTELLAR GRAINS Structure, formation STAR FORMATION Cloud collapse, protostellar formation, molecular outflows.

76. 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/

Search for: Current Category Everything What's new Top Searches Statistics Science News ... Home Current location: Astronomy > Interstellar Medium Emission Nebulae Planetary Nebulae Reflection Nebulae The Web Nebulae The Web Nebulae http://seds.lpl.arizona.edu/billa/twn/top.html detailed information Rating: [7.00] Votes: [344] Colorado Model of the Local Interstellar Cloud The hydrogen cloud in which the Solar System is immersed. 3D pictures of the cloud, view from any direction, movie, calculate hydrogen http://casa.colorado.edu/~sredfiel/ColoradoLIC.html detailed information Rating: [6.00] Votes: [2190] Interstellar Medium Learning pages About ISM from history of observation to current status of understanding. http://www-ssg.sr.unh.edu/tof/Outreach/Interstellar/ detailed information Rating: [6.00] Votes: [1334] Interstellar Molecules evolutionary cycle Evolutionary cycle of Interstellar Organic Molecules - Fullerenes, PAHs, Polyyenes, and biomolecules. http://www.shantanurastogi.homestead.com/files/ismol.html

77. 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

English Dictionary Computer Dictionary Thesaurus Dream Dictionary ... Medical Dictionary Search Dictionary: INTERSTELLAR MEDIUM: Dictionary Entry and Meaning WordNet Dictionary Definition: [n] interstellar space including streams ... stars See Also: interstellar space HOME ABOUT HYPERDICTIONARY

78. 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

Astronomy 162: Professor Barbara Ryden Tuesday, January 21 INTERSTELLAR MEDIUM ``They cannot scare me with their empty spaces Between stars - on stars where no human race is. I have it in me so much nearer home To scare myself with my own desert places.'' - Robert Frost Key Concepts The interstellar medium consists of low-density gas and dust. Interstellar gas consists of cool clouds embedded in hot intercloud gas. The interstellar medium emits, absorbs, and reflects radiation. (1) The interstellar medium (that's just a fancy name for the matter between stars) consists of low-density gas and dust. 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.

79. 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

Next: Protostellar Collapse and Disk Up: Scientific Motivation Previous: Scientific Motivation The Interstellar Medium 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.

80. 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

Next: The molecular medium in Up: RESEARCH Previous: Near infrared variability observations The Interstellar Medium . Other directions covering the star formation regions and molecular clouds in our own Galaxy as well as in other galaxies are presented here. The molecular medium in external galaxies (A. Andersson, H. Olofsson) Interstellar filaments and fragments (G. Gahm, A. Kaas, H. Kristen)

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