Be X-ray binaries in the SMC as indicators of mass-transfer efficiency
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Be X-ray binaries in the SMC as indicators of mass-transfer efficiency. / Vinciguerra, Serena; Neijssel, Coenraad J.; Vigna-Gomez, Alejandro; Mandel, Ilya; Podsiadlowski, Philipp; Maccarone, Thomas J.; Nicholl, Matt; Kingdon, Samuel; Perry, Alice; Salemi, Francesco.
In: Monthly Notices of the Royal Astronomical Society, Vol. 498, No. 4, 04.09.2020, p. 4705-4720.Research output: Contribution to journal › Journal article › Research › peer-review
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T1 - Be X-ray binaries in the SMC as indicators of mass-transfer efficiency
AU - Vinciguerra, Serena
AU - Neijssel, Coenraad J.
AU - Vigna-Gomez, Alejandro
AU - Mandel, Ilya
AU - Podsiadlowski, Philipp
AU - Maccarone, Thomas J.
AU - Nicholl, Matt
AU - Kingdon, Samuel
AU - Perry, Alice
AU - Salemi, Francesco
PY - 2020/9/4
Y1 - 2020/9/4
N2 - Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) with simulated populations of BeXRB-like systems produced with the COMPAS population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stablemass transfer, theirmass distribution suggests that at least similar to 30 per cent of themass donated by the progenitor of the NS is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the SMC shows that the excess of BeXRBs is most likely explained by this galaxy's burst of star formation similar to 20-40 Myr ago.
AB - Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) with simulated populations of BeXRB-like systems produced with the COMPAS population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stablemass transfer, theirmass distribution suggests that at least similar to 30 per cent of themass donated by the progenitor of the NS is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the SMC shows that the excess of BeXRBs is most likely explained by this galaxy's burst of star formation similar to 20-40 Myr ago.
KW - X-rays: binaries
KW - stars: emission-line
KW - Be
KW - stars: neutron
KW - stars: evolution
KW - gravitational waves
KW - methods: data analysis
KW - SMALL-MAGELLANIC-CLOUD
KW - NEUTRINO-DRIVEN EXPLOSIONS
KW - STAR-FORMATION CONDITIONS
KW - DOUBLE WHITE-DWARFS
KW - POPULATION SYNTHESIS
KW - PRESUPERNOVA EVOLUTION
KW - SUPERNOVA SIMULATIONS
KW - STELLAR EVOLUTION
KW - FORMATION HISTORY
KW - CLOSE BINARIES
U2 - 10.1093/mnras/staa2177
DO - 10.1093/mnras/staa2177
M3 - Journal article
VL - 498
SP - 4705
EP - 4720
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 4
ER -
ID: 252293130