Binary Population Synthesis: Low- and Intermediate-Mass X-Ray Binarie

Podsiadlowski, Ph.; Rappaport, S.; Pfahl, Eric

doi:10.1007/978-94-015-9723-4_26

Cited by 9 publications

(4 citation statements)

References 31 publications

(30 reference statements)

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“…Could they be the end products of low-mass X-ray binaries with a hidden neutron star in this system? Podsiadlowski et al (2001) suggests that the end products are predominantly He and low-mass hybrid HeCO WDs. When the pulsar beam is not pointing towards us, there would not be any direct detection of the neutron star.…”

Section: Unseen Companion(s)mentioning

confidence: 99%

First discovery of an ultra-cool white dwarf benchmark in common proper motion with an M dwarf

Lam

Hambly

Lodieu

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Ultra-cool white dwarfs are among the oldest stellar remnants in the Universe. Their efficient gravitational settling and low effective temperatures are responsible for the smooth spectra they exhibit. For that reason, it is not possible to derive their radial velocities or to find the chemistry of the progenitors. The best that can be done is to infer such properties from associated sources, which are coeval. The simplest form of such a system is a common proper motion pair where one star is an evolved degenerate and the other a main sequence star. In this work we present the discovery of the first of such a system, the M dwarf LHS 6328 and the ultra-cool white dwarf PSO J1801+625, from the Pan-STARRS 1 3π survey and the Gaia Data Release 2. Follow-up spectra were collected covering a usable wavelength range of 3750 to 24500Å. Their spectra show that the white dwarf has an effective temperature of 3550 K and surface gravity of log g = 7.45 ± 0.13 or log g = 7.49 ± 0.13 for a CO or He core, respectively, when compared against synthetic spectra of ultra-cool white dwarf atmosphere models. The system has slightly sub-solar metallicity with −0.25 < [Fe/H] < 0.0, and a spatial velocity of (U, V, W) = (−114.26 ± 0.24, 222.94 ± 0.60, 10.25 ± 0.34) km s −1 , the first radial velocity and metallicity measurements of an ultra-cool white dwarf. This makes it the first and only benchmark of its kind to date.

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Section: Unseen Companion(s)mentioning

confidence: 99%

First discovery of an ultra-cool white dwarf benchmark in common proper motion with an M dwarf

Lam

Hambly

Lodieu

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The possibility of a planet surviving its host star's supernova is often neglected, because a planet in orbit around a single exploding star is not expected to survive the supernova [5]. The combination of mass loss in the supernova explosion [6] and the natal kick imparted to the new compact object [7,8] mediates the survivability of low-mass x-ray binaries [9][10][11][12][13][14][15], but planetary orbits are too fragile to survive this process [16].…”

Section: Introductionmentioning

confidence: 99%

Lucky planets: how circum-binary planets survive the supernova in one of the inner-binary components

Auer

Zwart

2022

SciPost Astro.

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A planet hardly ever survives the supernova of the host star in a bound orbit, because mass loss in the supernova and the natal kick imparted to the newly formed compact object cause the planet to be ejected. A planet in orbit around a binary has a considerably higher probability to survive the supernova explosion of one of the inner binary stars. In those cases, the planet most likely remains bound to the companion of the exploding star, whereas the compact object is ejected. We estimate this to happen to \sim 1/33∼1/33 the circum-binary planetary systems. These planetary orbits tend to be highly eccentric (e \ {\raise-.5ex\hbox{>}}\ 0.9), and \sim 20∼20,% of these planets have retrograde orbits compared to their former binary. The probability that the planet as well as the binary (now with a compact object) remains bound is about ten times smaller (\sim 3\cdot 10^{-3}∼3⋅10−3). We then expect the Milky way Galaxy to host \ {\raise-.5ex\hbox{<}}\ 10 x-ray binaries that are still orbited by a planet, and \\ {\raise-.5ex\hbox{<}}\ 150 planets that survived in orbit around the compact object’s companion. These numbers should be convolved with the fraction of massive binaries that is orbited by a planet.

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“…The possibility that a planet survives a supernova is therefore generally ignored in studies on the origin of planets around pulsars (for instance in [10]). There is, however, a small but finite probability that the kick prevents the system from being ionized, this effect is considered important for the survivability of low-mass x-ray binaries [11][12][13][14][15]. Although, this might works effectively for low-mass x-ray binaries, the binding energy of an orbiting planet is considerably lower, and therefore the planet is easily lost.…”

Section: Introductionmentioning

confidence: 99%

Lucky planets: how circum-binary planets survive the supernova in one of the inner-binary components

Auer,

Zwart

2021

Preprint

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Since the discovery of exoplanets around pulsars, there has been a debate on their origin. Popular scenarios include in situ formation or the dynamical capture of a planet in a dense stellar system. The possibility of a planet surviving its host star's supernova is often neglected, because a planet in orbit around a single exploding star is not expected to survive the supernova. A circum-binary planet, however, may stand a chance in staying bound when one of the binary components explodes. We investigate the latter and constrain the distribution of post-supernova orbital parameters of circum-binary planets. This is done by performing population synthesis calculations of binary stars until the first supernova. Just before the supernova, we add a planet in orbit around the binary to study its survivability. In our supernova model, the exploding star's mass is assumed to change instantaneously, and we apply a velocity kick to the newly formed remnant. The mass loss and velocity kick affect the orbits of the two stars and the planet. Only 2 • 10 −3 of systems survive the supernova while keeping the circum-binary planet bound. The surviving planetary orbits are wide (a > ∼ 10 au) and eccentric (e > ∼ 0.3). It turns out much more likely (3 • 10 −2 system fraction) that the newly formed compact object is ejected from the system, leaving the planet bound to its companion star in a highly eccentric orbit (typically > ∼ 0.9). We expect that the Milky way Galaxy hosts at most 10 x-ray binaries that are still orbited by a planet, and < ∼ 150 planets that survived in orbit around the compact object's companion. These numbers should be convolved with the fraction of massive binaries that is orbited by a planet.

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Binary Population Synthesis: Low- and Intermediate-Mass X-Ray Binarie

Cited by 9 publications

References 31 publications

First discovery of an ultra-cool white dwarf benchmark in common proper motion with an M dwarf

First discovery of an ultra-cool white dwarf benchmark in common proper motion with an M dwarf

Lucky planets: how circum-binary planets survive the supernova in one of the inner-binary components

Lucky planets: how circum-binary planets survive the supernova in one of the inner-binary components

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