TY - JOUR
T1 - GW 150914-like black holes as Galactic high-energy sources
AU - Ioka, Kunihito
AU - Matsumoto, Tatsuya
AU - Teraki, Yuto
AU - Kashiyama, Kazumi
AU - Murase, Kohta
N1 - Funding Information:
We thank Takashi Nakamura, Tsvi Piran and Masaru Shibata for helpful comments. Thiswork is supported byKAKENHI24103006, 24000004, 26247042, 26287051, 17H01126, 17H06131, 17H06362, 17H06357 (KI), 17K14248 (KK), Grant-in-Aid for JSPS Research Fellow 17J09895 (TM) and by NSF Grant No. PHY-1620777 (KM). The authors also thank the Yukawa Institute for Theoretical Physics at Kyoto University. Discussions during the Long-term and Nishinomiya-Yukawa memorial workshop YITP-T-16-02 on 'Nuclear Physics, Compact Stars, and Compact Star Mergers 2016' were useful to complete this work.
Publisher Copyright:
© 2018 The Author(s).
PY - 2017/9/21
Y1 - 2017/9/21
N2 - The first direct detections of gravitational waves (GWs) from black hole (BH) mergers, GW 150914, GW 151226 and LVT 151012, give a robust lower limit ~70 000 -61 000+170 000 on the number of merged, highly spinning BHs in our Galaxy. The total spin energy is comparable to all the kinetic energy of supernovae that ever happened in our Galaxy. The BHs release the spin energy to relativistic jets by accreting matter and magnetic fields from the interstellar medium (ISM). By considering the distributions of the ISM density, BHmass and velocity, we calculate the luminosity function of the BH jets, and find that they can potentially accelerate TeV-PeV cosmic ray particles in our Galaxy with total power ~1037 ± 3 erg s-1 as PeVatrons, positron factories and/or unidentified TeV gamma-ray sources. Additional ~300 BH jet nebulae could be detectable by Cherenkov Telescope Array. We also argue that the accretion from the ISM can evaporate and blow away cold material around the BH, which has profound implications for some scenarios to predict electromagnetic counterparts to BH mergers.
AB - The first direct detections of gravitational waves (GWs) from black hole (BH) mergers, GW 150914, GW 151226 and LVT 151012, give a robust lower limit ~70 000 -61 000+170 000 on the number of merged, highly spinning BHs in our Galaxy. The total spin energy is comparable to all the kinetic energy of supernovae that ever happened in our Galaxy. The BHs release the spin energy to relativistic jets by accreting matter and magnetic fields from the interstellar medium (ISM). By considering the distributions of the ISM density, BHmass and velocity, we calculate the luminosity function of the BH jets, and find that they can potentially accelerate TeV-PeV cosmic ray particles in our Galaxy with total power ~1037 ± 3 erg s-1 as PeVatrons, positron factories and/or unidentified TeV gamma-ray sources. Additional ~300 BH jet nebulae could be detectable by Cherenkov Telescope Array. We also argue that the accretion from the ISM can evaporate and blow away cold material around the BH, which has profound implications for some scenarios to predict electromagnetic counterparts to BH mergers.
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U2 - 10.1093/MNRAS/STX1337
DO - 10.1093/MNRAS/STX1337
M3 - Article
AN - SCOPUS:85038618569
SN - 0035-8711
VL - 470
SP - 3332
EP - 3345
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -