Evolutionary Sequences For Low- And-Intermediate-Mass X-Ray Binaries Ph. Podsiadlowski S. Rappaport...
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Transcript of Evolutionary Sequences For Low- And-Intermediate-Mass X-Ray Binaries Ph. Podsiadlowski S. Rappaport...
![Page 1: Evolutionary Sequences For Low- And-Intermediate-Mass X-Ray Binaries Ph. Podsiadlowski S. Rappaport E. D. Pfahl.](https://reader036.fdocuments.in/reader036/viewer/2022070413/5697bfe91a28abf838cb6def/html5/thumbnails/1.jpg)
Evolutionary Sequences For Low-And-Intermediate-Mass
X-Ray Binaries
Ph. Podsiadlowski
S. Rappaport
E. D. Pfahl
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Introduction
• LMXBs: discovered 40 yr ago• Porb<10 days• No luminous companion stars• The only one case confirmed: Cyg X-2• LMXBs may descend from IMXBs
⊙MM donor 76.0~
dayshrPin 1004~
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Binary Calculations
• Roche lobe radius:
• Mass transfer rate:
• Angular momentum loss:
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• Angular momentum loss:
Binary Calculations
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(1): Systems evolving to long periods
(2): Systems evolving to short periods
(3): More massive systems Experiencing dynamical
mass transfer and spiral-in
Very few systems should be observable in the early
rapid phase and X-ray binaries are mostly likely to have a relatively low mass
secondary when they are observerd at the present
epoch
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Thermal Timescale Mass Transfer
• Mass-radius exponents:
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In radiative stars, a large fraction of the envelope (in radius) contains very
little mass
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The systems becomestemporarily detached when the H-burningshell stars to move
into the region with agradient in hydrogen
abundance,established duringthe hydrogen coreburning phase andthe giant shrinks
significantly
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The early mass transfer phase can bedivided into two separate phases:(1):a phase of atmospheric Roche
lobe overflow where the mass transfer rate increases exponentially,(2): a phase where the high-entropy material in the low-density envelope
of the secondary is lost
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The drop in Pmin at 13 hr occurs for amodel where the secondary has just exhausted hydrogen in the center at
the beginning of mass transfer
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Application to The Population of X-Ray Binaries
• Issues: (1) how unique are the evolutionary paths we have found, (2) are types of systems suggested by other reso
nably long-lived phases of our binary evolutions represented in the observed binary X-ray source population
(3) is our complete ensemble of binary evoltuion models consistent with the overall population of observed LMXBs and IMXBs?
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Application to Binary Millisecond Pulsars
In the Galaxy plane, binary radio pulsars classes:
(1):one major class involves systems with low-mass companions.
(2):the ones with substantially more massive white dwarf companions
(3):systems containing planetary mass companions
(4):systems consist of a pair of neutron stars
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A outstanding problem: the birthrate problem
Application to Binary Millisecond Pulsars