饮料
发表于 2025-3-23 13:11:53
,-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
exhilaration
发表于 2025-3-23 16:23:59
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.
vector
发表于 2025-3-23 19:12:46
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.
季雨
发表于 2025-3-23 22:50:04
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
Panacea
发表于 2025-3-24 03:59:05
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改进
发表于 2025-3-24 09:11:14
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.
异端邪说2
发表于 2025-3-24 14:23:01
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.
太空
发表于 2025-3-24 18:12:12
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).
出处
发表于 2025-3-24 22:59:21
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.
LIMIT
发表于 2025-3-25 03:12:43
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