The origin of the high-mass X-ray binary 4U 2206+54/BD+532790
Jan 19, 202211 pages
Published in:
- Mon.Not.Roy.Astron.Soc. 511 (2022) 3, 4123-4133
- Published: Mar 21, 2022
e-Print:
- 2201.07770 [astro-ph.SR]
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Abstract: (Oxford University Press)
Based on the Gaia EDR3 astrometric parameters and our new systemic radial velocity of the high-mass X-ray binary 4U 2206+54/BD+532790, we studied the trace back motion of the system and propose that it originated in the subgroup of the Cepheus OB1 association (Age ∼4–10 Myr) with its brightest star, BD+532820 (B0V; L∼10^4.7L_⊙). The kinematic age of 4U 2206+54 is about 2.8 ± 0.4 Myr, it is at a distance of 3.1–3.3 kpc and has a space velocity of 75–100 km s^−1 with respect to this member star (BD+532820) of the Cep OB1 association. This runaway velocity indicates that the progenitor of the neutron star hosted by 4U 2206+54 lost about 4–9 M_⊙ during the supernova explosion and the latter one received a kick velocity of at least 200–350 km s^−1 . Since the high-mass X-ray binary 4U 2206+54/BD+532790 was born as a member of a subgroup of Cep OB1, the initially most massive star in the system terminated its evolution within ≲7−9 Myr, corresponding to an initial mass ≳32 M_⊙.Note:
- 11 pages, 10 figures, accepted for publication in MNRAS
- stars: individual: HMXB 4U 2206+54/BD+53 2790
- X-ray: binaries
- stars: formation
- stars: evolution
- stars: neutron
- stars: supernovae
References(85)
Figures(10)