標(biāo)題: Titlebook: Astrophysics of the Diffuse Universe; Michael A. Dopita,Ralph S. Sutherland Textbook 2003 Springer-Verlag Berlin Heidelberg 2003 Astrochem [打印本頁(yè)] 作者: 切口 時(shí)間: 2025-3-21 17:34
書目名稱Astrophysics of the Diffuse Universe影響因子(影響力)
書目名稱Astrophysics of the Diffuse Universe影響因子(影響力)學(xué)科排名
書目名稱Astrophysics of the Diffuse Universe網(wǎng)絡(luò)公開度
書目名稱Astrophysics of the Diffuse Universe網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Astrophysics of the Diffuse Universe被引頻次
書目名稱Astrophysics of the Diffuse Universe被引頻次學(xué)科排名
書目名稱Astrophysics of the Diffuse Universe年度引用
書目名稱Astrophysics of the Diffuse Universe年度引用學(xué)科排名
書目名稱Astrophysics of the Diffuse Universe讀者反饋
書目名稱Astrophysics of the Diffuse Universe讀者反饋學(xué)科排名
作者: employor 時(shí)間: 2025-3-21 21:25 作者: Ischemia 時(shí)間: 2025-3-22 00:55 作者: VEIL 時(shí)間: 2025-3-22 08:36
Line Transfer Effects,la. However, whether the observer can see the emission depends upon whether the nebula is optically thick or optically thin to the escape of this radiation. This in turn depends upon the ., .., of the nebula at the frequency .. For transmission of light through an absorbing screen of material, the o作者: MAIM 時(shí)間: 2025-3-22 11:02 作者: 知道 時(shí)間: 2025-3-22 14:34 作者: anniversary 時(shí)間: 2025-3-22 17:50 作者: 獎(jiǎng)牌 時(shí)間: 2025-3-23 00:01 作者: 鑲嵌細(xì)工 時(shí)間: 2025-3-23 05:09 作者: 即席 時(shí)間: 2025-3-23 08:07
Parameters of Photoionized Regions, a wide variety of photoionized plasmas ranging from normal H. regions, planetary nebulae, and nova shells to much more exotic objects such as photoionizing shocks in metal-rich supernova remnants or active galaxies.作者: Intervention 時(shí)間: 2025-3-23 11:15
Photoionizing Shocks,st shocks, produce copious amounts of EUV or soft X-ray photons. These escape both upstream and downstream to be absorbed in either a precursor photoionized zone or in a narrow photoionized zone adjacent to the recombination region of the shock. In very fast shocks, the photon spectrum may be quite 作者: gruelling 時(shí)間: 2025-3-23 15:44
Interstellar Dust,l bulge of faint Galactic stars is crossed by dark lanes, filaments, and clouds of dense dusty gas made visible in projection. Because the dust grains are very small, typically less than a micron in diameter, their absorption characteristics are very wavelength dependent, and blue or ultraviolet pho作者: 健談的人 時(shí)間: 2025-3-23 19:34 作者: Functional 時(shí)間: 2025-3-24 01:43 作者: CAGE 時(shí)間: 2025-3-24 04:12
Foundation Game Design with ActionScript 3.0d wind. Within the disks of spiral galaxies, dusty clouds of molecular gas continually coalesce and collapse under their self-gravity to form new stars. The light from these newborn stars heats and ionizes their placental cloud before finally dispersing it back into the galactic disk, ready to repea作者: 延期 時(shí)間: 2025-3-24 07:47
Foundation Game Design with Flashpectra. A basic understanding of these is essential, since it is through the atomic and molecular lines that we ultimately derive our understanding about the physical conditions in, and chemical abundances of, diffuse astrophysical plasmas. In what follows, we will assume that the reader is familiar作者: Prognosis 時(shí)間: 2025-3-24 12:36 作者: 大都市 時(shí)間: 2025-3-24 16:51 作者: 精確 時(shí)間: 2025-3-24 20:24 作者: 畏縮 時(shí)間: 2025-3-25 01:23
Platform Game: Physics and Data Management,cific energies. These nearly monochromatic photons form the line emission or absorption of astrophysical plasmas. These bound levels arise as a consequence of the quantum-mechanical description and represent the quantized solutions for electrons bound to a nucleus in some form of potential. Above th作者: conscribe 時(shí)間: 2025-3-25 07:16 作者: 好忠告人 時(shí)間: 2025-3-25 10:37 作者: 弄皺 時(shí)間: 2025-3-25 13:00
Platform Game: Physics and Data Management,ming from a photoionizing source, be it a star, a nucleus of an active galaxy, or whatever. Such photoionization-dominated plasmas are very commonly observed in galaxies and historically, were one of the first to be studied in detail, thanks to their bright and prominent emission line spectra at opt作者: Endometrium 時(shí)間: 2025-3-25 19:26 作者: Capture 時(shí)間: 2025-3-25 23:09 作者: audiologist 時(shí)間: 2025-3-26 03:14
Controlling a Player Character,l bulge of faint Galactic stars is crossed by dark lanes, filaments, and clouds of dense dusty gas made visible in projection. Because the dust grains are very small, typically less than a micron in diameter, their absorption characteristics are very wavelength dependent, and blue or ultraviolet pho作者: BUMP 時(shí)間: 2025-3-26 05:12
Platform Game: Physics and Data Management, crisscrossed by violent shocks and pervaded by intense UV and X-ray radiation fields, which can easily tear apart delicate molecular bonds. Even the composition of the interstellar medium presents a problem to the formation of complex molecules, since the gas is mostly hydrogen and helium. Reactive作者: CANDY 時(shí)間: 2025-3-26 10:52
https://doi.org/10.1007/978-1-4302-4717-3which form new stars, new winds, and new supernovae in their turn, it is roiled, churned, and compressed to produce a ramified skein of cooler atomic or molecular gas embedded in hotter ionized phases. The spatial structure of these various thermal phases is driven by the interstellar gas seeking to作者: 熱心 時(shí)間: 2025-3-26 14:03 作者: Servile 時(shí)間: 2025-3-26 20:03 作者: Nomadic 時(shí)間: 2025-3-26 21:08 作者: faultfinder 時(shí)間: 2025-3-27 01:33
Parameters of Photoionized Regions, a wide variety of photoionized plasmas ranging from normal H. regions, planetary nebulae, and nova shells to much more exotic objects such as photoionizing shocks in metal-rich supernova remnants or active galaxies.作者: 神圣將軍 時(shí)間: 2025-3-27 08:40 作者: Lime石灰 時(shí)間: 2025-3-27 11:55
978-3-642-07771-5Springer-Verlag Berlin Heidelberg 2003作者: 主動(dòng)脈 時(shí)間: 2025-3-27 13:45
Astrophysics of the Diffuse Universe978-3-662-05866-4Series ISSN 0941-7834 Series E-ISSN 2196-9698 作者: 出沒 時(shí)間: 2025-3-27 18:01
Platform Game: Physics and Data Management,ming from a photoionizing source, be it a star, a nucleus of an active galaxy, or whatever. Such photoionization-dominated plasmas are very commonly observed in galaxies and historically, were one of the first to be studied in detail, thanks to their bright and prominent emission line spectra at optical wavelengths.作者: 組裝 時(shí)間: 2025-3-28 00:43
Advanced Object and Character Control, a wide variety of photoionized plasmas ranging from normal H. regions, planetary nebulae, and nova shells to much more exotic objects such as photoionizing shocks in metal-rich supernova remnants or active galaxies.作者: 制造 時(shí)間: 2025-3-28 04:06 作者: Itinerant 時(shí)間: 2025-3-28 06:42 作者: 新字 時(shí)間: 2025-3-28 12:06 作者: 急性 時(shí)間: 2025-3-28 17:08
Textbook 2003i- tions, chemical makeup and, evolution of the (thermal) interstellar medium. We hope it provides an up-to-date overview which postgraduates, advanced undergraduates, and professionals in astrophysics can use as a "reference of first resort" before going on to read the more specialist monographs or作者: 侵蝕 時(shí)間: 2025-3-28 22:16
https://doi.org/10.1007/978-1-4302-1822-7ar theory. The Saha equation describes a different equilibrium from the coronal approximation because in LTE, the excited states are all populated according to Boltzmann’s law. These excited states play an important role in determining the ionization state of the medium.作者: 土坯 時(shí)間: 2025-3-29 00:15 作者: ABHOR 時(shí)間: 2025-3-29 05:22 作者: Debility 時(shí)間: 2025-3-29 09:01
Continuum and Recombination Line Processes,of a continuum of free states. Nevertheless, electrons can still make transitions between these free states, known as free-free transitions, or between bound atomic levels and free states, known as bound-free or free-bound transitions. In this nomenclature, the line transitions discussed so far are bound-bound transitions.作者: escalate 時(shí)間: 2025-3-29 14:21
Foundation Game Design with Flash with the basic concepts of quantum mechanics. If not, the reader is referred to the highly readable account of this and other topics in modern physics which is in the book by Rohlf (1994). Also, a lucid introduction to molecular spectroscopy is given by Atkins (1983); see notes on this chapter.作者: 繁忙 時(shí)間: 2025-3-29 18:17 作者: 寬敞 時(shí)間: 2025-3-29 21:57 作者: 縮短 時(shí)間: 2025-3-30 02:16
0941-7834 iffuse universe.Astrophysics is treated as a practical appliOur purpose in writing this book is to show how physics has been applied to developing our current understanding of the phase structure, physical condi- tions, chemical makeup and, evolution of the (thermal) interstellar medium. We hope it 作者: 裂縫 時(shí)間: 2025-3-30 07:19 作者: overrule 時(shí)間: 2025-3-30 09:27 作者: morale 時(shí)間: 2025-3-30 15:45
Cooling Plasmas,oling through different processes. These are collisional excitation cooling through emission lines (..), cooling through collisional ionization losses (..), heating through recombinations (..), cooling through continuum emission processes (..), heating by photoionization (..), and Compton heating or cooling (..).作者: 不足的東西 時(shí)間: 2025-3-30 16:54
Thermal Phases of Diffuse Matter,or molecular gas embedded in hotter ionized phases. The spatial structure of these various thermal phases is driven by the interstellar gas seeking to attain a pressure balance and a dynamic balance between heating and cooling. Many of these phases are in a stochastic pressure balance with one another.作者: 靦腆 時(shí)間: 2025-3-31 00:47 作者: cortex 時(shí)間: 2025-3-31 01:34
What Is the Diffuse Universe?,e briefly as their shock energy is radiated away. In clusters of galaxies, heated gas glows softly in X-rays, cooling over billions of years before finally falling back into the bright galaxy cores to help feed the massive monster black holes that lurk at their centers. In intergalactic space, jets 作者: 我要威脅 時(shí)間: 2025-3-31 08:28 作者: 招致 時(shí)間: 2025-3-31 10:51
Photoionizing Shocks, (8.77). Here instead we take the timescale for the flow to cool to 104 K from the immediate hot postshock region. By the time the plasma has dropped to this temperature, all the photionizing radiation can be generated by the cooling plasma has been radiated, upstream and downstream. This is at a po作者: 直言不諱 時(shí)間: 2025-3-31 15:04
Interstellar Dust,ed, either by magnetic fields or some other agency such as radiation pressure or mechanical effects, to produce a direction-dependent extinction which polarizes the light in transmission or scattering.作者: 描繪 時(shí)間: 2025-3-31 19:04
Introduction to Astrochemistry,ar species can be built up. In this chapter, we will simply get a taste for these phenomena. To find out more, the recent book by Emma Bakes (1997), and the reviews by Dalgarno (1987) and Genzel (1992) are strongly recommended (see notes on this chapter).
