標(biāo)題: Titlebook: An Introduction to the Evolution of Single and Binary Stars; Matthew Benacquista Textbook 2013 Springer Science+Business Media New York 20 [打印本頁] 作者: otitis-externa 時(shí)間: 2025-3-21 19:41
書目名稱An Introduction to the Evolution of Single and Binary Stars影響因子(影響力)
書目名稱An Introduction to the Evolution of Single and Binary Stars影響因子(影響力)學(xué)科排名
書目名稱An Introduction to the Evolution of Single and Binary Stars網(wǎng)絡(luò)公開度
書目名稱An Introduction to the Evolution of Single and Binary Stars網(wǎng)絡(luò)公開度學(xué)科排名
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書目名稱An Introduction to the Evolution of Single and Binary Stars讀者反饋
書目名稱An Introduction to the Evolution of Single and Binary Stars讀者反饋學(xué)科排名
作者: breadth 時(shí)間: 2025-3-22 00:04 作者: 狂熱文化 時(shí)間: 2025-3-22 03:39 作者: amyloid 時(shí)間: 2025-3-22 05:33 作者: 臭名昭著 時(shí)間: 2025-3-22 08:50 作者: 彎曲的人 時(shí)間: 2025-3-22 15:06 作者: 壟斷 時(shí)間: 2025-3-22 19:31 作者: 自由職業(yè)者 時(shí)間: 2025-3-22 21:13 作者: 盡管 時(shí)間: 2025-3-23 04:55
,Einleitung – zum Anliegen der Arbeit,is contained within ～ 60 . of the radius. For lower-mass stars, this extends out to about 80 % of the radius. Naturally, the energy production is significantly higher in high-mass stars and extends out to larger radii.作者: 某人 時(shí)間: 2025-3-23 07:36
https://doi.org/10.1007/978-3-476-03840-1 baryon structure changes, altering their cooling process. Neutron stars are frequently born with high magnetic fields that slowly decay and spin down the neutron star. Black holes, however, will not change much for eons. In this chapter, we will look at the properties and continued evolution of these exotic objects.作者: 核心 時(shí)間: 2025-3-23 10:34 作者: Inflamed 時(shí)間: 2025-3-23 14:21
Classifying and Describing Starsdinate system. We begin by describing some bulk motions of the more prominent objects in the sky. From there we describe the subtle motions of the stars and the coordinate system used to locate them. We conclude with a system for describing the brightness of stars.作者: resilience 時(shí)間: 2025-3-23 21:03
Introduction to Binary Systemsnary stars. We will begin by describing the orbit of a binary and how these orbits are observed. We conclude this chapter with a discussion of how stellar masses are obtained from observations of the spectra of binary stars.作者: 莊嚴(yán) 時(shí)間: 2025-3-24 00:25 作者: 短程旅游 時(shí)間: 2025-3-24 02:43
Compact Remnants baryon structure changes, altering their cooling process. Neutron stars are frequently born with high magnetic fields that slowly decay and spin down the neutron star. Black holes, however, will not change much for eons. In this chapter, we will look at the properties and continued evolution of these exotic objects.作者: Lacunar-Stroke 時(shí)間: 2025-3-24 06:47
Dynamical Evolution of Binariesder to provide the energy needed to halt core collapse. In addition, single stars can combine through strong interactions in order to form new binaries. In this final chapter, we will look at the ways in which dynamical interactions within clusters can alter the population of binary stellar systems within the cluster.作者: 原來 時(shí)間: 2025-3-24 13:36 作者: COW 時(shí)間: 2025-3-24 15:16 作者: 暫時(shí)休息 時(shí)間: 2025-3-24 21:24
Textbook 2013 with a background and introduction of basic astronomical concepts. Although a general treatment of stellar structure and evolution is included, the text stresses the physical processes that lead to stellar mass compact object binaries that may be sources of observable gravitational radiation. .Basi作者: vanquish 時(shí)間: 2025-3-24 23:56
Classifying and Describing Stars by others. In other words, we need to develop a .. Generally, when developing a coordinate system, we look for landmarks to which can anchor the coordinate system. We begin by describing some bulk motions of the more prominent objects in the sky. From there we describe the subtle motions of the sta作者: creditor 時(shí)間: 2025-3-25 03:50
Introduction to Binary Systemsthat stellar models are meant to replicate. Some of our data comes from observations of nearby single stars, but much of our information comes from binary stars. We will begin by describing the orbit of a binary and how these orbits are observed. We conclude this chapter with a discussion of how ste作者: 半導(dǎo)體 時(shí)間: 2025-3-25 09:53
Measuring Other Stellar Propertiesand light curves of binary systems allow us to determine the temperatures, sizes, and luminosities of many nearby stars. In this way we can find correlations between different stellar properties and begin to sort stars into different categories and classifications.作者: 紅潤 時(shí)間: 2025-3-25 14:35 作者: 鼓掌 時(shí)間: 2025-3-25 16:38
Nuclear Processes in a volume a few femtometers across. The strong nuclear force that interacts with nucleons and binds them must be stronger than the repulsive electrostatic force that the protons feel in such close proximity to each other. The nuclear force cannot be long range or it would draw all nucleons in the作者: 無表情 時(shí)間: 2025-3-25 23:53 作者: 群居男女 時(shí)間: 2025-3-26 04:08 作者: 潔凈 時(shí)間: 2025-3-26 06:51
Main Sequence Structure structure can be discovered through these solutions. The mass distribution indicates that for high-mass stars with . ≥ 1. 2 M. over 95 % of the mass is contained within ～ 60 . of the radius. For lower-mass stars, this extends out to about 80 % of the radius. Naturally, the energy production is sign作者: tariff 時(shí)間: 2025-3-26 11:55
Compact Remnantspped in these objects, they each continue to evolve in ways that are unique to their structure. As white dwarfs cool and become more degenerate, their baryon structure changes, altering their cooling process. Neutron stars are frequently born with high magnetic fields that slowly decay and spin down作者: ZEST 時(shí)間: 2025-3-26 16:34
Binary Evolutionthe spherical symmetry that was assumed in the development of the evolution equations in Chap.?4 and then used in later chapters. For the most part, these additional considerations do not significantly alter the evolution of the components of a binary since the orbital periods are generally greater 作者: Brittle 時(shí)間: 2025-3-26 20:32 作者: 積云 時(shí)間: 2025-3-26 23:48 作者: decode 時(shí)間: 2025-3-27 02:22 作者: Filibuster 時(shí)間: 2025-3-27 09:04 作者: 小卷發(fā) 時(shí)間: 2025-3-27 11:55 作者: 消息靈通 時(shí)間: 2025-3-27 16:20
,Vertr?ge, Abkommen und Vereinbarungen,In order to solve the evolution equations [Eqs.?(4.36)–(4.38)] for the variables ρ, ., and ., we need to be able to express the auxiliary functions ., ., and . in terms of these variables. Additional physics must be included to accomplish this.作者: Armory 時(shí)間: 2025-3-27 21:51
https://doi.org/10.1007/978-3-658-05823-4Now that we have an understanding of the physics behind both the equations of stellar structure and their auxiliary functions, we are in a position to describe some simple static models of stellar structure.作者: 調(diào)情 時(shí)間: 2025-3-27 22:38
Stellar Evolution EquationsWe want to develop models of stellar evolution that can reproduce the mass–luminosity relation as well as the structure of the H-R diagram. Obviously, we will start with several simplifying assumptions that can be relaxed as we try to achieve better fidelity to observations.作者: Panther 時(shí)間: 2025-3-28 05:38 作者: Indelible 時(shí)間: 2025-3-28 09:36 作者: narcissism 時(shí)間: 2025-3-28 14:16
https://doi.org/10.1007/978-3-662-33272-6 by others. In other words, we need to develop a .. Generally, when developing a coordinate system, we look for landmarks to which can anchor the coordinate system. We begin by describing some bulk motions of the more prominent objects in the sky. From there we describe the subtle motions of the sta作者: Mhc-Molecule 時(shí)間: 2025-3-28 15:22
https://doi.org/10.1007/978-3-662-33272-6that stellar models are meant to replicate. Some of our data comes from observations of nearby single stars, but much of our information comes from binary stars. We will begin by describing the orbit of a binary and how these orbits are observed. We conclude this chapter with a discussion of how ste作者: Foreshadow 時(shí)間: 2025-3-28 20:05
https://doi.org/10.1007/978-3-662-42542-8and light curves of binary systems allow us to determine the temperatures, sizes, and luminosities of many nearby stars. In this way we can find correlations between different stellar properties and begin to sort stars into different categories and classifications.作者: PHAG 時(shí)間: 2025-3-29 00:52 作者: 殘忍 時(shí)間: 2025-3-29 05:30
Die deutsch-polnischen Beziehungen 1949–2000 in a volume a few femtometers across. The strong nuclear force that interacts with nucleons and binds them must be stronger than the repulsive electrostatic force that the protons feel in such close proximity to each other. The nuclear force cannot be long range or it would draw all nucleons in the作者: 光明正大 時(shí)間: 2025-3-29 07:34
Die deutsch-tschechischen Europaregionenpencil balanced on its point is also in equilibrium, but it is not stable against small perturbations. We now need to consider when our equilibrium solutions are also stable against small perturbations. In so doing, we will encounter a number of potential instabilities that may have a significant ef作者: Hangar 時(shí)間: 2025-3-29 13:38 作者: 陪審團(tuán)每個(gè)人 時(shí)間: 2025-3-29 16:52
,Einleitung – zum Anliegen der Arbeit, structure can be discovered through these solutions. The mass distribution indicates that for high-mass stars with . ≥ 1. 2 M. over 95 % of the mass is contained within ～ 60 . of the radius. For lower-mass stars, this extends out to about 80 % of the radius. Naturally, the energy production is sign作者: ZEST 時(shí)間: 2025-3-29 21:22
https://doi.org/10.1007/978-3-476-03840-1pped in these objects, they each continue to evolve in ways that are unique to their structure. As white dwarfs cool and become more degenerate, their baryon structure changes, altering their cooling process. Neutron stars are frequently born with high magnetic fields that slowly decay and spin down作者: Aesthete 時(shí)間: 2025-3-30 02:38 作者: Spinal-Tap 時(shí)間: 2025-3-30 07:37
https://doi.org/10.1007/978-3-662-33269-6pressure from the ignition of bright massive stars and the pressure waves from the following supernovae can sweep away residual mass in the cloud. In some cases, the cluster will become unbound due to the loss of mass. The constituent stars of the cluster are then scattered and they continue to evol作者: 過多 時(shí)間: 2025-3-30 08:33 作者: 煤渣 時(shí)間: 2025-3-30 13:01
An Introduction to the Evolution of Single and Binary Stars978-1-4419-9991-7Series ISSN 2192-4791 Series E-ISSN 2192-4805 作者: 物種起源 時(shí)間: 2025-3-30 19:12 作者: 多產(chǎn)子 時(shí)間: 2025-3-30 22:35
,Europ?ische Priorit?t, 1974 bis 1981,e time exploring the envelopes of stars. We will revisit the energy density and pressure due to radiation and discuss the consequences of local thermodynamic equilibrium. Finally, we will also look in more detail at the nature of absorption lines in stellar spectra.作者: 主講人 時(shí)間: 2025-3-31 02:12
Die deutsch-tschechischen Europaregionenpencil balanced on its point is also in equilibrium, but it is not stable against small perturbations. We now need to consider when our equilibrium solutions are also stable against small perturbations. In so doing, we will encounter a number of potential instabilities that may have a significant effect in the structure and evolution of stars.作者: Arthr- 時(shí)間: 2025-3-31 07:46 作者: Canvas 時(shí)間: 2025-3-31 12:57 作者: CAJ 時(shí)間: 2025-3-31 14:17
