Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013
We present Monitor of All-sky X-ray Image (MAXI) and Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the Be X-ray binary, MAXI J0655−013, in outburst. NuSTAR observed the source once early in the outburst, when spectral analysis yields a bolometric (0.1–100 keV), unabsorbed source lum...
| Main Authors: | , , , , , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2023-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ace696 |
| _version_ | 1797694408201601024 |
|---|---|
| author | Sean N. Pike Mutsumi Sugizaki Jakob van den Eijnden Benjamin Coughenour Amruta D. Jaodand Tatehiro Mihara Sara E. Motta Hitoshi Negoro Aarran W. Shaw Megumi Shidatsu John A. Tomsick |
| author_facet | Sean N. Pike Mutsumi Sugizaki Jakob van den Eijnden Benjamin Coughenour Amruta D. Jaodand Tatehiro Mihara Sara E. Motta Hitoshi Negoro Aarran W. Shaw Megumi Shidatsu John A. Tomsick |
| author_sort | Sean N. Pike |
| collection | DOAJ |
| description | We present Monitor of All-sky X-ray Image (MAXI) and Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the Be X-ray binary, MAXI J0655−013, in outburst. NuSTAR observed the source once early in the outburst, when spectral analysis yields a bolometric (0.1–100 keV), unabsorbed source luminosity of L _bol = 5.6 × 10 ^36 erg s ^−1 , and a second time 54 days later, by which time the luminosity had dropped to L _bol = 4 × 10 ^34 erg s ^−1 after first undergoing a dramatic increase. Timing analysis of the NuSTAR data reveals a neutron star spin period of 1129.09 ± 0.04 s during the first observation, which decreased to 1085 ± 1 s by the time of the second observation, indicating spin-up due to accretion throughout the outburst. Furthermore, during the first NuSTAR observation, we observed quasi-periodic oscillations (QPOs) with centroid frequency ν _0 = 89 ± 1 mHz, which exhibited a second harmonic feature. By combining the MAXI and NuSTAR data with pulse period measurements reported by Fermi/GBM, we are able to show that apparent flaring behavior in the MAXI light curve is an artifact introduced by uneven sampling of the pulse profile, which has a large pulsed fraction. Finally, we estimate the magnetic field strength at the neutron star surface via three independent methods, invoking a tentative cyclotron resonance scattering feature at 44 keV, QPO production at the inner edge of the accretion disk, and spin-up via interaction of the neutron star magnetic field with accreting material. Each of these result in a significantly different value. We discuss the strengths and weaknesses of each method and infer that MAXI J0655−013 is likely to have a high surface magnetic field strength, B _s > 10 ^13 G. |
| first_indexed | 2024-03-12T02:57:26Z |
| format | Article |
| id | doaj.art-c1b71db6a01e422588ee05ae26a8a0ec |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T02:57:26Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-c1b71db6a01e422588ee05ae26a8a0ec2023-09-03T15:13:18ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195414810.3847/1538-4357/ace696Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013Sean N. Pike0https://orcid.org/0000-0002-8403-0041Mutsumi Sugizaki1https://orcid.org/0000-0002-1190-0720Jakob van den Eijnden2https://orcid.org/0000-0002-5686-0611Benjamin Coughenour3https://orcid.org/0000-0003-0870-6465Amruta D. Jaodand4https://orcid.org/0000-0002-3850-6651Tatehiro Mihara5https://orcid.org/0000-0002-6337-7943Sara E. Motta6https://orcid.org/0000-0002-6154-5843Hitoshi Negoro7https://orcid.org/0000-0003-0939-1178Aarran W. Shaw8https://orcid.org/0000-0002-8808-520XMegumi Shidatsu9https://orcid.org/0000-0001-8195-6546John A. Tomsick10https://orcid.org/0000-0001-5506-9855Department of Astronomy and Astrophysics, University of California , San Diego, CA 92093, USA ; snpike@ucsd.eduNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Beijing 100012, People’s Republic of ChinaDepartment of Physics, University of Warwick , Coventry, CV4 7AL, UKSpace Sciences Laboratory, 7 Gauss Way, University of California , Berkeley, CA 94720-7450, USACahill Center for Astronomy and Astrophysics, California Institute of Technology , 1200 E California Boulevard, Pasadena, CA 91125, USAHigh Energy Astrophysics Laboratory , RIKEN, 2-1, Hirosawa, Wako, Saitama 351-0198, JapanIstituto Nazionale di Astrofisica , Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate (LC), Italy; Department of Physics, Astrophysics, University of Oxford , Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UKDepartment of Physics, Nihon University , 1-8-14 Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308, JapanDepartment of Physics, University of Nevada , Reno, NV 89557, USADepartment of Physics, Ehime University , 2-5, Bunkyocho, Matsuyama, Ehime 790-8577, JapanSpace Sciences Laboratory, 7 Gauss Way, University of California , Berkeley, CA 94720-7450, USAWe present Monitor of All-sky X-ray Image (MAXI) and Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the Be X-ray binary, MAXI J0655−013, in outburst. NuSTAR observed the source once early in the outburst, when spectral analysis yields a bolometric (0.1–100 keV), unabsorbed source luminosity of L _bol = 5.6 × 10 ^36 erg s ^−1 , and a second time 54 days later, by which time the luminosity had dropped to L _bol = 4 × 10 ^34 erg s ^−1 after first undergoing a dramatic increase. Timing analysis of the NuSTAR data reveals a neutron star spin period of 1129.09 ± 0.04 s during the first observation, which decreased to 1085 ± 1 s by the time of the second observation, indicating spin-up due to accretion throughout the outburst. Furthermore, during the first NuSTAR observation, we observed quasi-periodic oscillations (QPOs) with centroid frequency ν _0 = 89 ± 1 mHz, which exhibited a second harmonic feature. By combining the MAXI and NuSTAR data with pulse period measurements reported by Fermi/GBM, we are able to show that apparent flaring behavior in the MAXI light curve is an artifact introduced by uneven sampling of the pulse profile, which has a large pulsed fraction. Finally, we estimate the magnetic field strength at the neutron star surface via three independent methods, invoking a tentative cyclotron resonance scattering feature at 44 keV, QPO production at the inner edge of the accretion disk, and spin-up via interaction of the neutron star magnetic field with accreting material. Each of these result in a significantly different value. We discuss the strengths and weaknesses of each method and infer that MAXI J0655−013 is likely to have a high surface magnetic field strength, B _s > 10 ^13 G.https://doi.org/10.3847/1538-4357/ace696High-mass x-ray binary starsNeutron starsAccretionPulsars |
| spellingShingle | Sean N. Pike Mutsumi Sugizaki Jakob van den Eijnden Benjamin Coughenour Amruta D. Jaodand Tatehiro Mihara Sara E. Motta Hitoshi Negoro Aarran W. Shaw Megumi Shidatsu John A. Tomsick Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013 The Astrophysical Journal High-mass x-ray binary stars Neutron stars Accretion Pulsars |
| title | Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013 |
| title_full | Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013 |
| title_fullStr | Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013 |
| title_full_unstemmed | Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013 |
| title_short | Accretion Spin-up and a Strong Magnetic Field in the Slow-spinning Be X-Ray Binary MAXI J0655-013 |
| title_sort | accretion spin up and a strong magnetic field in the slow spinning be x ray binary maxi j0655 013 |
| topic | High-mass x-ray binary stars Neutron stars Accretion Pulsars |
| url | https://doi.org/10.3847/1538-4357/ace696 |
| work_keys_str_mv | AT seannpike accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT mutsumisugizaki accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT jakobvandeneijnden accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT benjamincoughenour accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT amrutadjaodand accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT tatehiromihara accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT saraemotta accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT hitoshinegoro accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT aarranwshaw accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT megumishidatsu accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 AT johnatomsick accretionspinupandastrongmagneticfieldintheslowspinningbexraybinarymaxij0655013 |