2020A&A...640A..86P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST09:28:52

2020A&A...640A..86P - Astronomy and Astrophysics, volume 640A, 86-86 (2020/8-1)

Kinematic distinction of the two subpopulations of X-ray pulsars.

PRISEGEN M.

Abstract (from CDS):


Context. The population of Be/X-ray binaries shows strong evidence of bimodality, especially in the spin period of neutron stars. Several physical mechanisms may produce this bimodality. The most favored candidate mechanisms are two distinct supernova channels or different accretion modes of the neutron stars in Be/X-ray binaries. Investigating the kinematics of these systems may provide some additional insight into the physics of this bimodality.
Aims. If the two Be/X-ray binary subpopulations arise from two distinct supernova types, then the two subpopulations should have different peculiar (systemic) velocities. This can be tested either directly, by measuring the velocity of the system, or indirectly, by measuring the position of the system with respect to its birthplace. A difference in the peculiar velocity magnitude between the subpopulations would favor the supernova hypothesis, and the lack of this difference would suggest that the accretion hypothesis is a more favorable option to explain the bimodality.
Methods. Using the most recent Gaia dataset and the newest catalogs of Small Magellanic Cloud (SMC) star clusters, we analyzed the tangential peculiar velocities of Be/X-ray binaries in the Galaxy and the positions of Be/X-ray binaries in the SMC. We used the distance of the system from the nearest young star cluster as a proxy to the tangential velocity of the system. We applied statistical testing to investigate whether the two subpopulations that are divided by the spin of the neutron star are also kinematically distinct.
Results. There is evidence that the two subpopulations are indeed kinematically distinct. However, the tangential peculiar velocities of the two subpopulations are the reverse from what is expected from the distinct supernova channel hypothesis. We find some marginal evidence (p≃0.005) that the Galactic Be/X-ray binaries from the short-spin subpopulation have systematically higher peculiar velocities than the systems from the long-spin subpopulation. The same effect, but weaker, is also recovered for the SMC Be/X-ray binaries for all considered cluster catalogs. The unexpected difference in the peculiar velocities between the two subpopulations of Be/X-ray binaries contradicts these two hypotheses, and an alternative physical explanation for this may be needed.

Abstract Copyright: © ESO 2020

Journal keyword(s): binaries: general - stars: neutron - X-rays: binaries

Simbad objects: 40

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Number of rows : 40

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9559 1
2 SK 160 HXB 01 17 05.1447530244 -73 26 36.015353425 12.23 13.00 13.15   13.17 O9.7Ia+ 801 0
3 V* V635 Cas HXB 01 18 31.9704429246 +63 44 33.071137750 17.05 16.64 15.19 14.34 13.22 B0.2Ve 669 0
4 EM* GGA 104 HXB 01 47 00.2121223849 +61 21 23.661992704 11.76 12.09 11.366 11.00 10.52 B1IIIe 172 0
5 2MASS J01581848+6713234 HXB 01 58 18.4910576029 +67 13 23.459737878 15.74 15.65 14.43 13.44 12.55 B2IVe+ 24 0
6 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5762 1
7 V* BQ Cam HXB 03 34 59.9116460415 +53 10 23.296351781   17.16 15.42 14.26 13.04 O8.5Ve 407 1
8 V* X Per HXB 03 55 23.0778791365 +31 02 45.045745259 6.090 6.840 6.720     O9.5III 909 0
9 LS V +44 17 HXB 04 40 59.3295352454 +44 31 49.258751047 11.02 11.42 10.73 10.28 9.76 B0.2Ve 99 0
10 HD 245770 HXB 05 38 54.5749436467 +26 18 56.839215267 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 879 0
11 PSR J0635+0533 Psr 06 35 17.4 +05 33 21   13.81 12.83     B1IIIe-B2Ve 40 0
12 2E 1752 HXB 06 58 17.2878555250 -07 12 35.203675058   12.38 10.9 11.40   O9.7Ve 73 0
13 V* V441 Pup HXB 07 28 53.5787769417 -26 06 28.895160996 11.27 12.29 11.83 11.53   O5Ve 69 0
14 V* V572 Pup HXB 08 12 28.3576629560 -31 14 52.138780764 12.14 13.03 12.74 12.44   B0.2IVe 62 0
15 Ginga 0834-430 HXB 08 35 55 -43 11.1     20.4     B0-2III-Ve 93 0
16 GRO J1008-571 HXB 10 09 46.9645132055 -58 17 35.603669270       14.63   B0e 175 0
17 LS 1698 HXB 10 37 35.3144388592 -56 47 55.866836619   12.00 11.48 11.38   B0III/V:e 95 0
18 WRAY 15-793 HXB 11 20 57.1736252056 -61 55 00.165172193 12.81 13.06 12.12     O9.5III/Ve 175 0
19 IGR J11435-6109 HXB 11 44 00.2944630617 -61 07 36.482240268       15.70   B2III/B0V 46 1
20 HD 102567 Be* 11 48 00.0214627917 -62 12 24.900348094 8.24 9.06 9.00 9.62   O/Bne 291 0
21 HD 110432 Be* 12 42 50.2655719413 -63 03 31.048323668 4.79 5.58 5.31     B0.5IVpe 272 0
22 V* V850 Cen HXB 13 01 17.0966951298 -61 36 06.636402972   15.6       B2Vne 276 0
23 [KRL2007b] 129 Psr 13 01 58.7203639191 -63 58 08.830169485           O9V/B1III 51 0
24 4U 1416-62 HXB 14 21 12.8 -62 41 54   17.9 17.2     B1Ve 126 0
25 HD 153295 HXB 17 00 25.2435284420 -42 19 00.280593627 9.05     9.52   B2e 70 0
26 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11760 0
27 2MASS J18453684+0051474 HXB 18 45 36.8356137141 +00 51 47.438374606     20.6     B0-2IV-Ve 104 0
28 4U 1901+03 HXB 19 03 39.3919805263 +03 12 15.742327187           OB 76 0
29 XTE J1906+090 HXB 19 04 47.491 +09 02 41.40           Be? 24 0
30 IGR J19294+1816 HXB 19 29 55.9035072710 +18 18 38.226053335           B1Ve 30 1
31 XTE J1946+274 HXB 19 45 39.3569004855 +27 21 55.502556930   18.76 16.92 15.62 14.38 B0-1IV-Ve 104 0
32 2MASS J19493548+3012317 HXB 19 49 35.4840244577 +30 12 31.775034731   15.16 14.22 13.53 12.88 B0Ve 138 1
33 V* V2246 Cyg HXB 20 32 15.2744631713 +37 38 14.839930326   22.16 19.41 17.32 15.18 B0Ve 380 0
34 GRO J2058+42 HXB 20 58 47.5371693693 +41 46 37.180557326   15.97 14.74 14.74 13.35 O9.5-B0IV-Ve 63 0
35 GSC 03588-00834 HXB 21 03 35.7101268891 +45 45 05.568943629   15.34 14.20 13.49 12.75 B0Ve 150 0
36 V* V490 Cep HXB 21 39 30.6903601561 +56 59 10.421972716   15.2       B1.5Ve 132 1
37 BD+53 2790 HXB 22 07 56.2368407539 +54 31 06.405811141 9.4 10.11 9.84 9.64 9.43 O9.5Vep 174 0
38 4U 2238+60 HXB 22 39 20.8444678371 +61 16 26.607919757   16.26 14.80 13.89 12.92 Be 44 0
39 HD 215227 Be* 22 42 57.30295 +44 43 18.2525 8.07 8.86 8.81     B1.5-B2III 86 1
40 2MASS J22535512+6243368 HXB 22 53 55.1259067421 +62 43 36.791537094 17.64 17.38 15.61 13.3 13.29 BIII 20 0

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2020.10.24-09:28:52

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