TY - JOUR

T1 - Testing the fossil field hypothesis

T2 - Could strongly magnetized OB stars produce all known magnetars?

AU - Холтыгин, Александр Федорович

AU - Makarenko, Ekaterina

AU - Igoshev, Andrei

PY - 2021/7/1

Y1 - 2021/7/1

N2 - Stars of spectral types O and B produce neutron stars (NSs) after supernova explosions. Most of NSs are strongly magnetised including normal radio pulsars with B~10^12 G and magnetars with B~10^14 G. A fraction of 7-12 per cent of massive stars are also magnetised with B~10^3 G and some are weakly magnetised with B~1 G. It was suggested that magnetic fields of NSs could be the fossil remnants of magnetic fields of their progenitors. This work is dedicated to study this hypothesis. First, we gather all modern precise measurements of surface magnetic fields in O, B and A stars. Second, we estimate parameters for log-normal distribution of magnetic fields in B stars and found mu_B = 2.83 ± 0.1 log10(G), sigma_B = 0.65 ± 0.09 for strongly magnetised and mu_B = 0.14 ± 0.5 log10(G), sigma_B = 0.7_-0.27^+0.57 for weakly magnetised. Third, we assume that the magnetic field of pulsars and magnetars have 2.7 DEX difference in magnetic fields and magnetars represent 10 per cent of all young NSs and run population synthesis. We found that it is impossible to simultaneously reproduce pulsars and magnetars populations if the difference in their magnetic fields is 2.7 DEX. Therefore, we conclude that the simple fossil origin of the magnetic field is not viable for NSs.

AB - Stars of spectral types O and B produce neutron stars (NSs) after supernova explosions. Most of NSs are strongly magnetised including normal radio pulsars with B~10^12 G and magnetars with B~10^14 G. A fraction of 7-12 per cent of massive stars are also magnetised with B~10^3 G and some are weakly magnetised with B~1 G. It was suggested that magnetic fields of NSs could be the fossil remnants of magnetic fields of their progenitors. This work is dedicated to study this hypothesis. First, we gather all modern precise measurements of surface magnetic fields in O, B and A stars. Second, we estimate parameters for log-normal distribution of magnetic fields in B stars and found mu_B = 2.83 ± 0.1 log10(G), sigma_B = 0.65 ± 0.09 for strongly magnetised and mu_B = 0.14 ± 0.5 log10(G), sigma_B = 0.7_-0.27^+0.57 for weakly magnetised. Third, we assume that the magnetic field of pulsars and magnetars have 2.7 DEX difference in magnetic fields and magnetars represent 10 per cent of all young NSs and run population synthesis. We found that it is impossible to simultaneously reproduce pulsars and magnetars populations if the difference in their magnetic fields is 2.7 DEX. Therefore, we conclude that the simple fossil origin of the magnetic field is not viable for NSs.

KW - stars: neutron

KW - magnetic fields

KW - stars:massive

KW - magnetars

KW - stars: magnetic field

KW - Methods: statistical

KW - Magnetic fields

KW - Methods: statistical

KW - Stars: magnetars

KW - Stars: magnetic field

KW - Stars: massive

KW - Stars: neutron

KW - MAGNETICALLY SPLIT LINES

KW - MASSIVE STARS

KW - AP STARS

KW - magnetic fields

KW - stars: magnetars

KW - B-TYPE STARS

KW - DELTA-SCUTI STAR

KW - POPULATION SYNTHESIS

KW - ISOLATED NEUTRON-STARS

KW - OBLIQUE ROTATOR MODEL

KW - stars: neutron

KW - methods: statistical

KW - stars: magnetic field

KW - STELLAR EVOLUTION

KW - stars: massive

KW - OBSERVED VELOCITY DISTRIBUTION

UR - http://www.scopus.com/inward/record.url?scp=85108619283&partnerID=8YFLogxK

UR - https://www.mendeley.com/catalogue/6702cbda-3b73-308d-aca2-b1ce26d32d46/

U2 - 10.1093/mnras/stab1175

DO - 10.1093/mnras/stab1175

M3 - Article

VL - 504

SP - 5813

EP - 5828

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -