標題: Titlebook: Cataclysmic Variables and Low-Mass X-Ray Binaries; Proceedings of the 7 Donald Q. Lamb,Joseph Patterson Conference proceedings 1985 D. Reid [打印本頁] 作者: mobility 時間: 2025-3-21 18:19
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書目名稱Cataclysmic Variables and Low-Mass X-Ray Binaries被引頻次
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書目名稱Cataclysmic Variables and Low-Mass X-Ray Binaries讀者反饋
書目名稱Cataclysmic Variables and Low-Mass X-Ray Binaries讀者反饋學(xué)科排名
作者: 清澈 時間: 2025-3-21 22:12 作者: OTTER 時間: 2025-3-22 00:44 作者: cortex 時間: 2025-3-22 07:14
Abell 41, A Cataclysmic Variable Progenitorwith its critical Roche surface in the astronomically near future initiating mass transfer and cataclysmic activity..The existence of this star provides direct evidence for theoretical work suggesting that binary stars which, have suffered catastrophic angular momentum loss through the ejection of a作者: 切掉 時間: 2025-3-22 09:30 作者: 外貌 時間: 2025-3-22 13:55
Galactic Bulge X-Ray Burst Sources from Disrupted Globular Clusters ?.? 19) G or K star is found within the error circle (3″ radius) in four cases. These may be surviving giants in a disrupted globular cluster core. Implications for globular cluster evolution and the GXRBS themselves are discussed.作者: 外貌 時間: 2025-3-22 18:31 作者: 沒有希望 時間: 2025-3-22 23:47 作者: 颶風(fēng) 時間: 2025-3-23 04:01 作者: 放縱 時間: 2025-3-23 06:02 作者: 飲料 時間: 2025-3-23 13:11
,-Inner Functions and ,-Contractions,systems whose orbital periods are greater than ?3., relative to shorter-period systems. This result may provide a natural explanation for the apparent sharp decrease in the discovery probability of h a see cataclysmic variable as its orbital period decreases through ?3. (see Fig. 2). However, the ef作者: exhilaration 時間: 2025-3-23 16:23
Anny M. S. Cheng,Scheffer C. G. Tseng.? 19) G or K star is found within the error circle (3″ radius) in four cases. These may be surviving giants in a disrupted globular cluster core. Implications for globular cluster evolution and the GXRBS themselves are discussed.作者: vector 時間: 2025-3-23 19:12
Alister Miskimmon,Ben O’Loughlin these systems, and report on calculations of their expected numbers. We also briefly discuss the relationship of highly compact binaries in globular clusters to the bright X-ray sources of the Galactic bulge.作者: 季雨 時間: 2025-3-23 22:50
0067-0057 Many of the meetings have been held - following a custom older than anyone reading this book - in locations with well-known recreational potential (e. g. Santa Cruz, CA; Boulder, CO). We thought hard about this custom while contemplating the possibility of organi- zing a meeting in Massachusetts in 作者: Panacea 時間: 2025-3-24 03:59 作者: 改進 時間: 2025-3-24 09:11
On The Evolutionary Status of Bright, Low-Mass X-Ray Sourceslation (Markers .. 1977; Van Speybroeck .. 1979). They have (at least in our own Galaxy) very similar X-ray flux distributions (Jones 1977), and lack the X-ray pulsations frequently found in massive X-ray binaries. Presumably, they are old, low-mass binaries in which the magnetic fields of the neutron stars have decayed.作者: 異端邪說2 時間: 2025-3-24 14:23
Overtraining Syndrome in Athletes magnetic stellar wind (MSW) is limited from below. The same MSW can explain the origin and, possibly, also the observed number of WUMa stars. Bright (L~10.-10.L.) X-ray sources may be members of binaries whose evolution is driven by this MSW.作者: 太空 時間: 2025-3-24 18:12
https://doi.org/10.1007/978-3-030-53153-9bservations (Cowley et al,1979). Such a long binary period is not consistent with the low-mass close binary model of Joss and Rappaport (1979); rather, it suggests that the primary is a somewhat evolved low-mass star (Cowley et at,1979).作者: 出處 時間: 2025-3-24 22:59
Magnetic Braking and the Origin and Evolution of Close Low-Mass Binaries magnetic stellar wind (MSW) is limited from below. The same MSW can explain the origin and, possibly, also the observed number of WUMa stars. Bright (L~10.-10.L.) X-ray sources may be members of binaries whose evolution is driven by this MSW.作者: LIMIT 時間: 2025-3-25 03:12 作者: 不如屎殼郎 時間: 2025-3-25 07:11 作者: 儲備 時間: 2025-3-25 09:42 作者: EWE 時間: 2025-3-25 14:14 作者: defeatist 時間: 2025-3-25 17:02
Conference proceedings 1985e meetings have been held - following a custom older than anyone reading this book - in locations with well-known recreational potential (e. g. Santa Cruz, CA; Boulder, CO). We thought hard about this custom while contemplating the possibility of organi- zing a meeting in Massachusetts in the middle作者: 柔美流暢 時間: 2025-3-26 00:01 作者: Ostrich 時間: 2025-3-26 01:21
Anny M. S. Cheng,Scheffer C. G. Tsengconfirmed by the detection of a dozen cataclysmic variables by the EINSTEIN X-ray satellite [8]. We show that the ratio of the formation rates of cataclysmic binaries and LMBX’s is appreciably smaller than the ratio of the number of white dwarfs to the number of neutron stars. A more detailed description of our work is given in [5].作者: 傀儡 時間: 2025-3-26 06:32
Evolution of Cataclysmic Binariesused by gravitational radiation and could produce R CrB stars, AM CVn cataclysmic binaries, DB white dwarfs, and Type I Supernovae. Inconsistencies in the standard evolutionary scenario are discussed. It is possible that a binary nature of a star is the necessary condition for a formation of a high surface brightness planetary nebula.作者: 有毛就脫毛 時間: 2025-3-26 08:31
Three Body Interactions and Cataclysmic Binaries in Globular Clustersconfirmed by the detection of a dozen cataclysmic variables by the EINSTEIN X-ray satellite [8]. We show that the ratio of the formation rates of cataclysmic binaries and LMBX’s is appreciably smaller than the ratio of the number of white dwarfs to the number of neutron stars. A more detailed description of our work is given in [5].作者: Diskectomy 時間: 2025-3-26 12:48
A Systematic Study of Magnetic Braking in Low-Mass Binariesal radiation (Rappaport .. 1982). We have extended this code by using a composite polytrope model for the secondary, wherein the structure of the radiative core is described by an n. = 3 polytrope and the convective envelope by an n = 3/2 polytrope. Our results are described in Rappaport .. 1983; this paper is a short summary.作者: 利用 時間: 2025-3-26 20:31
Low-Mass X-Ray Binariesof the sun’s disk in Figure 1. This is the smallest known LMXB; the optical companion is slightly larger than the sunspot group and the bow-tie shaped accretion disk is the same size as Saturn’s ring system.作者: Malleable 時間: 2025-3-27 00:25
The Mass Transfer Rate in X1916-053: Is it Driven by Gravitational Radiation?xpected from gravitational radiation (GR). Within uncertainty of a factor of 2 the transfer rate for the composite model solution is consistent with GR, but enhancement by other mechanisms should be investigated.作者: 繁重 時間: 2025-3-27 03:52 作者: infringe 時間: 2025-3-27 06:42 作者: 宣稱 時間: 2025-3-27 12:38 作者: 玷污 時間: 2025-3-27 13:48 作者: misanthrope 時間: 2025-3-27 19:29 作者: 可憎 時間: 2025-3-27 22:38
Alister Miskimmon,Ben O’Loughlinects, is presented. The resulting appearance is compared to recent observations of X-ray dips in several X-ray binaries. We also discuss the dynamical effects of X-ray induced mass loss, which originates at large radius in the disk.作者: Negligible 時間: 2025-3-28 02:38 作者: Mendicant 時間: 2025-3-28 09:00 作者: 軟弱 時間: 2025-3-28 12:50 作者: 大包裹 時間: 2025-3-28 14:53 作者: Cytokines 時間: 2025-3-28 19:03
Hydrodynamic Simulations of a Combined Hydrogen, Helium Thermonuclear Runaway on a 10 Km Neutron Sta1.0M, 10 km neutron star. Our simulation produced an outburst which lasted about 2000 sec and peak effective temperature was 3 kev. The peak luminosity exceeded 2 x 10. L . A shock wave caused a precursor in the light curve which lasted 10. sec.作者: 細頸瓶 時間: 2025-3-29 02:40
COS-B X-Ray Observations of Cygnus X-3220 days the total duration of observation of this source by COS-B. Preliminary results from the last observations are presented which show that:.The last point does not allow to confirm the hypothesis of an apsidal motion as the cause of the short-term changes of the 4.8h period.作者: PRISE 時間: 2025-3-29 04:54 作者: 外表讀作 時間: 2025-3-29 09:39
The So-What? Making Sense of It All,elope” phase. If this is the case, there should exist a class of detached “pre-cataclysmic” binaries: double nuclei of planetary nebulae, and close binaries containing hot subdwarfs or white dwarfs. The secondary stars should be lower-main-sequence objects, and the orbital periods should be short (<作者: FLORA 時間: 2025-3-29 12:01 作者: disrupt 時間: 2025-3-29 18:59
,-Inner Functions and ,-Contractions,ing the techniques developed by Rappaport, Joss, and Webbink (1982). Our new calculations (see Fig. 1) take into account the combined effects of (i) the gradual breakdown of quasi-equilibrium of the .He abundance in the interior of the secondary, and (ii) the progressive mixture of fresh .He into th作者: 劇毒 時間: 2025-3-29 23:10
New Findings on Overtraining Syndrome,ay sources (Verbunt and Zwaan 1981). A simplified stellar evolution code, which describes the mass-losing star as an n= 3/2 polytrope, was developed previously to study the evolution of binaries with a secondary of low mass (0.01 < M/M. < 0.4), when the angular momentum losses are due to gravitation作者: faucet 時間: 2025-3-29 23:56 作者: Stress 時間: 2025-3-30 05:01 作者: Antagonism 時間: 2025-3-30 08:12 作者: 斷言 時間: 2025-3-30 14:22
Anny M. S. Cheng,Scheffer C. G. Tsengct that many (or most) of the GX sources are x-ray burst sources (GXRBS) and are otherwise apparently identical to the luminous x-ray sources found in globular cluster cores implies that they too may have a globular cluster origin. The possibility that the compact x-ray binaries found in globulars a作者: gout109 時間: 2025-3-30 17:50 作者: 瑣事 時間: 2025-3-31 00:17
Alister Miskimmon,Ben O’Loughlinch binaries are subject to the combined influences of gravitational radiation, thermal evolution of the secondary star, gradual mass transfer from the secondary to the collapsed object primary when the system is in contact, and occasional gravitational encounters with field stars, some of which caus作者: Wordlist 時間: 2025-3-31 04:34 作者: 駕駛 時間: 2025-3-31 05:25 作者: 革新 時間: 2025-3-31 11:17 作者: GRUEL 時間: 2025-3-31 16:50 作者: 諷刺 時間: 2025-3-31 19:55 作者: 偏見 時間: 2025-4-1 00:30
