[PDF] Top 20 Interrupted Binary Mass Transfer in Star Clusters
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Interrupted Binary Mass Transfer in Star Clusters
... mean binary separation during MT, which dominates the 1 + 2 cross-section but not the 2 + 2 cross- section, since the mean binary separation in the cluster is much larger than the mean binary ... See full document
6
Hydrodynamics of Mass Transfer and Accretion in Close Binary Systems With Compact Objects
... X-ray binary systems, most of them Be X-ray binaries, are character- ized by rather large orbital ...the binary system, suggesting instead that the X-ray flares are related to the orbital dynamics of the ... See full document
185
Mass Transfer in Binary Stellar Evolution and Its Stability
... low mass X-ray binary system (LMXBs), one has a highly evolved, compact star (CVs and LMXBs contain white dwarfs and neutron stars, respectively) and a less evolved main sequence or red giant ... See full document
20
The evolution and masses of the neutron star and donor star in the high mass X-ray binary OAO1657-415
... Ofpe/WN9 star in this system, although significantly hydrogen depleted, has retained a small fraction of its ...which mass transfer occurs in a short binary orbit in which the secondary is the ... See full document
8
Post common envelope binaries from SDSS IV, SDSS J121258 25–012310 1, a new eclipsing system
... in binary or multiple star systems and a large fraction of binaries will interact at some point in their ...massive star reaches the RGB or the AGB. If the mass transfer rate is high ... See full document
10
Old star clusters: Bench tests of low mass stellar models
... of star cluster TO and White Dwarf (WD) ages has very recently confirmed the efficiency of a new physical process at work in the interior of ...WD+WD binary systems, the progeny of a ∼ 50% primordial ... See full document
9
Accreting neutron stars and black holes
... a binary millisecond radio pulsar, from an initial binary containing a massive supergiant and a low-mass star ...massive star evolves much faster than its companion and is the first to ... See full document
174
Hillenbrand_2018_AJ_155_51.pdf
... candidate binary star systems in the Pleiades, Praesepe, and NGC 2264 star clusters, based on robotic adaptive optics imaging data obtained using Robo-AO at the Palomar 60 ″ ...candidate ... See full document
15
How do binary clusters form?
... of star clusters are found in pairs, known as binary ...for binary cluster formation; we use N-body simu- lations to show that velocity substructure in a single (even fairly smooth) region can ... See full document
11
The photometric period in ES Ceti
... In order to address this issue, we have conducted a long-term timing study of the AM CVn star ES Ceti (Warner & Woudt 2002). This system shows a 620-s optical modulation which is complex in structure and ... See full document
7
Young, Massive Star Clusters in the Antennae
... the clusters in our sample were initially identified by the Ks band flux-limited ...the clusters were detected as part of spectroscopic observations of other ...the clusters originally identified in ... See full document
158
Optical identification of IGR J19140+0951
... Abstract. IGR J19140+0951 was discovered by INTEGRAL in 2003 in the 4-100 keV band. Observations with INTEGRAL and RXTE provide a tentative identification as a high-mass X-ray binary (HMXB) with a neutron ... See full document
7
An accurate mass and radius measurement for an ultracool white dwarf
... Therefore, since we knew the mass ratio from our spectro- scopic observations we could use it as a prior constraint and hence we were able to measure these parameters simulta- neously. Unfortunately, this approach ... See full document
10
The hunt for red dwarf binaries and hot planets in the WFCAM transit survey.
... a star- forming cloud collapses, it fragments into low-number multiple systems, which can be broken up by dynamical interactions ...during binary formation, driving the mass-ratio to unity ...of ... See full document
185
Evolution of star clusters on eccentric orbits
... lution of properties of clusters on eccentric orbits by that of clusters on circular orbits. This is useful for modelling techniques that are not able to include orbital eccentricity, such as the ... See full document
7
How does a low-mass cut-off in the stellar IMF affect the evolution of young star clusters?
... the star cluster ...cluster mass loss is ...a star formally escapes the star cluster at a distance r from the cluster centre at a radial orbit with velocity v, then it will be identified as an ... See full document
12
Simulations of stripped core-collapse supernovae in close binaries
... companion star, but we also see an increase in the den- sity in a ring surrounding the hole, as shown most clearly in Figure ...companion star, where material is stripped and swept up with the ejecta, this ... See full document
19
d182ab3a50e05ea2376a3f24d0b73b50558d3019.pdf
... Chevalier & Clegg ( 1985 ) made the fi rst analytic model of how stellar winds from multiple stars can merge to completely alter the ISM. Over the fi rst few Myr of a starburst, OB star winds in fl ate bubbles of ... See full document
13
The environmental dependence of the stellar mass function at z ~ 1. Comparing cluster and field between the GCLASS and UltraVISTA surveys
... The structure of the paper is as follows. In Sect. 2 we give an overview of GCLASS, and the spectroscopic and photometric data that have been taken for this cluster sample. We also de- scribe the data from the reference ... See full document
18
The radial velocity of the companion star in the low mass X ray binary 2S 0921 630 : limits on the mass of the compact object
... companion star. The K1 template star (HD 124106) spectrum veiled by an accretion disc contribution of 80 per ...companion star have been identified below the average spectrum at phase ... See full document
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