Distribution of High-Mass X-Ray Binaries in the Milky Way

Coleiro, A.; Chaty, S.

doi:10.1088/0004-637x/764/2/185

Cited by 77 publications

(63 citation statements)

References 65 publications

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“…The resulting systemic velocities are therefore also small with an average of vsys ≃ 10 km s −1 . This picture seems to have observational support when considering the typical small migration distances (∼ 0.1 kpc) of HMXBs from the spiral arms in the Milky Way (Coleiro & Chaty 2013).…”

Section: Location Of Ultra-stripped Sne In Host Galaxiesmentioning

confidence: 62%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

417

613

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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Section: Location Of Ultra-stripped Sne In Host Galaxiesmentioning

confidence: 62%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

417

613

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“…Adding new identifications by Coleiro & Chaty (2013) and Fortin et al (2017), we find that the total number of HMXBs currently known in our Galaxy amounts to 167. These sources thus represent ∼ 43% of the total number of high-energy binary systems, i.e.…”

Section: Rlo-hmxbsmentioning

confidence: 92%

“…These sources thus represent ∼ 43% of the total number of high-energy binary systems, i.e. adding all known LMXBs and HMXBs reported in Liu et al (2007), Coleiro & Chaty (2013), Bird et al (2016) and Fortin et al (2017), respectively. Among the 167 HMXBs, there are 70 firmly identified BeHMXBs, 35 sgHMXBs (including 12 SFXTs), 3 RLO-HMXBs, and 59 HMXBs of unidentified nature (Fortin et al 2017).…”

Section: Rlo-hmxbsmentioning

confidence: 99%

“…Contrary to LMXBs (which have lost traces of their precise birth), HMXBs are concentrated in the Galactic plane, toward tangential directions of Galactic arms, rich in star-forming regions and stellar complexes (Coleiro & Chaty 2013, and references therein). The distribution of HMXBs in any galaxy is thus a good indicator of star formation activity, and their collective X-ray luminosity has been used to compute the starformation rate of their host galaxy (Grimm et al 2003).…”

Section: Rlo-hmxbsmentioning

confidence: 99%

“…The distribution of HMXBs in any galaxy is thus a good indicator of star formation activity, and their collective X-ray luminosity has been used to compute the starformation rate of their host galaxy (Grimm et al 2003). Coleiro & Chaty (2013) have correlated the position of Galactic HMXBs (including BeHMXBs and sgHMXBs) with the position of star-forming complexes (SFCs), and showed that HMXBs are clustered within 0.3 kpc of a SFC, with an inter-cluster distance of 1.7 kpc, thus showing that HMXBs remain close to their birth place (see also Bodaghee et al 2012, who found a slightly larger average offset between HMXBs and OB associations, but still consistent within error bars of Coleiro & Chaty (2013)). As we shall discuss later, in connection to the kinematics of DNS systems (Section 6), this is an important finding for constraining the magnitude of the kick velocity imparted on the resulting NS formed in the first SN explosion.…”

Section: Rlo-hmxbsmentioning

confidence: 99%

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Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

641

690

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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2015

Pulsating Stars

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Distribution of High-Mass X-Ray Binaries in the Milky Way

Cited by 77 publications

References 65 publications

Ultra-stripped supernovae: progenitors and fate

Ultra-stripped supernovae: progenitors and fate

Formation of Double Neutron Star Systems

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