Kinematic distinction of the two subpopulations of X-ray
pulsars

J 2020

Kinematic distinction of the two subpopulations of X-ray pulsars

PRIŠEGEN, Michal

Základní údaje

Originální název

Kinematic distinction of the two subpopulations of X-ray pulsars

Autoři

PRIŠEGEN, Michal

Vydání

Astronomy and Astrophysics, Les Ulis, EDP Sciences, 2020, 0004-6361

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL

Impakt faktor

Impact factor: 5.803

Kód RIV

RIV/00216224:14310/20:00116236

Organizační jednotka

Přírodovědecká fakulta

DOI

https://doi.org/10.1051/0004-6361/201935642

UT WoS

000564318500004

EID Scopus

2-s2.0-85090402901

Klíčová slova anglicky

binaries: general; stars: neutron; X-rays: binaries

Štítky

14312040, rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 21. 1. 2021 14:28, Mgr. Marie Novosadová Šípková, DiS.

Anotace

V originále

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 approximate to 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.

Návaznosti

MUNI/A/0877/2019, interní kód MU

Název: Studium pokročilých problémů v oblasti teoretické fyziky, astrofyziky a fyzikálního vzdělávání

Investor: Masarykova univerzita, Studium pokročilých problémů v oblasti teoretické fyziky, astrofyziky a fyzikálního vzdělávání, DO R. 2020_Kategorie A - Specifický výzkum - Studentské výzkumné projekty

Citovat

PRIŠEGEN, Michal. Kinematic distinction of the two subpopulations of X-ray pulsars. Astronomy and Astrophysics. Les Ulis: EDP Sciences, 2020, roč. 640, August 2020, s. 1-15. ISSN 0004-6361. Dostupné z: https://doi.org/10.1051/0004-6361/201935642.

@article{1674716,
   author = {Prišegen, Michal},
   article_location = {Les Ulis},
   article_number = {August 2020},
   doi = {https://doi.org/10.1051/0004-6361/201935642},
   keywords = {binaries: general; stars: neutron; X-rays: binaries},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Kinematic distinction of the two subpopulations of X-ray pulsars},
   url = {https://doi.org/10.1051/0004-6361/201935642},
   volume = {640},
   year = {2020}
}

TY  - JOUR
ID  - 1674716
AU  - Prišegen, Michal
PY  - 2020
TI  - Kinematic distinction of the two subpopulations of X-ray pulsars
JF  - Astronomy and Astrophysics
VL  - 640
IS  - August 2020
SP  - 1-15
EP  - 1-15
PB  - EDP Sciences
SN  - 00046361
KW  - binaries: general
KW  - stars: neutron
KW  - X-rays: binaries
UR  - https://doi.org/10.1051/0004-6361/201935642
L2  - https://doi.org/10.1051/0004-6361/201935642
N2  - 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 approximate to 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.
ER  -

PRIŠEGEN, Michal. Kinematic distinction of the two subpopulations of X-ray pulsars. \textit{Astronomy and Astrophysics}. Les Ulis: EDP Sciences, 2020, roč.~640, August 2020, s.~1-15. ISSN~0004-6361. Dostupné z: https://doi.org/10.1051/0004-6361/201935642.

Přehled o publikaci