Titlebook: Cataclysmic Variables and Low-Mass X-Ray Binaries; Proceedings of the 7 Donald Q. Lamb,Joseph Patterson Conference proceedings 1985 D. Reid

饮料

,-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

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

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

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

改进

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

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

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

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