MULTI-WAVELENGTH EMISSIONS FROM THE MILLISECOND PULSAR BINARY PSR J1023+0038 DURING AN ACCRETION ACTIVE STATE
Recent observations strongly suggest that the millisecond pulsar binary PSR J1023+0038 has developed an accretion disk since 2013 June. We present a multi-wavelength analysis of PSR J1023+0038, which reveals that (1) its gamma-rays suddenly brightened within a few days in 2013 June/July and has rema...
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| Veröffentlicht in: | The Astrophysical journal 2014-04, Vol.785 (2), p.1-8 |
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| creator | Takata, J Li, K L Leung, Gene C K Kong, A K H Tam, P H T Hui, C Y Wu, E M H Xing, Yi Cao, Yi Tang, Sumin Wang, ZhongXiang Cheng, K S |
| description | Recent observations strongly suggest that the millisecond pulsar binary PSR J1023+0038 has developed an accretion disk since 2013 June. We present a multi-wavelength analysis of PSR J1023+0038, which reveals that (1) its gamma-rays suddenly brightened within a few days in 2013 June/July and has remained at a high gamma-ray state for several months; (2) both UV and X-ray fluxes have increased by roughly an order of magnitude; and (3) the spectral energy distribution has changed significantly after the gamma-ray sudden flux change. Time variabilities associated with UV and X-rays are on the order of 100-500 s and 50-100 s, respectively. Our model suggests that a newly formed accretion disk, due to the sudden increase of the stellar wind, could explain the changes of all these observed features. The increase of UV is emitted from the disk, and a new component in gamma-rays is produced by inverse Compton scattering between the new UV component and pulsar wind. The increase of X-rays results from the enhancement of injection pulsar wind energy into the intra-binary shock due to the increase of the stellar wind. We also predict that the radio pulses may be blocked by the evaporated winds from the disk, and the pulsar is still powered by rotation. |
| doi_str_mv | 10.1088/0004-637X/785/2/131 |
| format | Article |
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We present a multi-wavelength analysis of PSR J1023+0038, which reveals that (1) its gamma-rays suddenly brightened within a few days in 2013 June/July and has remained at a high gamma-ray state for several months; (2) both UV and X-ray fluxes have increased by roughly an order of magnitude; and (3) the spectral energy distribution has changed significantly after the gamma-ray sudden flux change. Time variabilities associated with UV and X-rays are on the order of 100-500 s and 50-100 s, respectively. Our model suggests that a newly formed accretion disk, due to the sudden increase of the stellar wind, could explain the changes of all these observed features. The increase of UV is emitted from the disk, and a new component in gamma-rays is produced by inverse Compton scattering between the new UV component and pulsar wind. The increase of X-rays results from the enhancement of injection pulsar wind energy into the intra-binary shock due to the increase of the stellar wind. We also predict that the radio pulses may be blocked by the evaporated winds from the disk, and the pulsar is still powered by rotation.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/785/2/131</identifier><language>eng</language><publisher>United States</publisher><subject>ACCRETION DISKS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; BINARY STARS ; COMPTON EFFECT ; EMISSION ; ENERGY SPECTRA ; Fluxes ; GAMMA RADIATION ; Inverse ; Millisecond pulsars ; PULSARS ; PULSES ; Spectral energy distribution ; STELLAR WINDS ; ULTRAVIOLET RADIATION ; WAVELENGTHS ; X RADIATION ; X-rays</subject><ispartof>The Astrophysical journal, 2014-04, Vol.785 (2), p.1-8</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c454t-6cbcac67d6fce32d1f0f80a0219fb41f121dce8e85d5254920b69ffd1d0d8ea83</citedby><cites>FETCH-LOGICAL-c454t-6cbcac67d6fce32d1f0f80a0219fb41f121dce8e85d5254920b69ffd1d0d8ea83</cites><orcidid>0000-0002-1262-7375 ; 0000-0003-1984-3852 ; 0000-0002-8036-8491 ; 0000-0002-6225-8918</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,777,781,882,27905,27906</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22357088$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Takata, J</creatorcontrib><creatorcontrib>Li, K L</creatorcontrib><creatorcontrib>Leung, Gene C K</creatorcontrib><creatorcontrib>Kong, A K H</creatorcontrib><creatorcontrib>Tam, P H T</creatorcontrib><creatorcontrib>Hui, C Y</creatorcontrib><creatorcontrib>Wu, E M H</creatorcontrib><creatorcontrib>Xing, Yi</creatorcontrib><creatorcontrib>Cao, Yi</creatorcontrib><creatorcontrib>Tang, Sumin</creatorcontrib><creatorcontrib>Wang, ZhongXiang</creatorcontrib><creatorcontrib>Cheng, K S</creatorcontrib><title>MULTI-WAVELENGTH EMISSIONS FROM THE MILLISECOND PULSAR BINARY PSR J1023+0038 DURING AN ACCRETION ACTIVE STATE</title><title>The Astrophysical journal</title><description>Recent observations strongly suggest that the millisecond pulsar binary PSR J1023+0038 has developed an accretion disk since 2013 June. We present a multi-wavelength analysis of PSR J1023+0038, which reveals that (1) its gamma-rays suddenly brightened within a few days in 2013 June/July and has remained at a high gamma-ray state for several months; (2) both UV and X-ray fluxes have increased by roughly an order of magnitude; and (3) the spectral energy distribution has changed significantly after the gamma-ray sudden flux change. Time variabilities associated with UV and X-rays are on the order of 100-500 s and 50-100 s, respectively. Our model suggests that a newly formed accretion disk, due to the sudden increase of the stellar wind, could explain the changes of all these observed features. The increase of UV is emitted from the disk, and a new component in gamma-rays is produced by inverse Compton scattering between the new UV component and pulsar wind. The increase of X-rays results from the enhancement of injection pulsar wind energy into the intra-binary shock due to the increase of the stellar wind. We also predict that the radio pulses may be blocked by the evaporated winds from the disk, and the pulsar is still powered by rotation.</description><subject>ACCRETION DISKS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>BINARY STARS</subject><subject>COMPTON EFFECT</subject><subject>EMISSION</subject><subject>ENERGY SPECTRA</subject><subject>Fluxes</subject><subject>GAMMA RADIATION</subject><subject>Inverse</subject><subject>Millisecond pulsars</subject><subject>PULSARS</subject><subject>PULSES</subject><subject>Spectral energy distribution</subject><subject>STELLAR WINDS</subject><subject>ULTRAVIOLET RADIATION</subject><subject>WAVELENGTHS</subject><subject>X RADIATION</subject><subject>X-rays</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><recordid>eNqNkTtPwzAUhS0EEuXxC1gssSChUD_ixBlDalqjNEVJymOyUscWRW1T4jDw70lUxMx0z5U-neF8AFxhdIcR52OEkO8FNHwdh5yNyRhTfARGmFHu-ZSFx2D0R5yCM-c-hpdE0Qhs58u0lN5L_CxSkU3LGRRzWRRykRXwIV_MYTkTcC7TVBYiWWQT-LRMiziH9zKL8zf4VOTwESNCbxGiHE6WucymMM5gnCS5KPuaPpXyWcCijEtxAU5stXHm8veeg-WDKJOZly6mMolTT_vM77xAr3Slg7AOrDaU1Ngiy1GFCI7syscWE1xrww1nNSPMjwhaBZG1Na5RzU3F6Tm4PvQ2rlsrp9ed0e-62e2M7hQh_ST9aj11c6D2bfP5ZVyntmunzWZT7Uzz5RQOMY-C0Kf0HyhiiJOQ-T1KD6huG-daY9W-XW-r9lthpAZbahhfDS5Ub0sR1duiP6iRfXA</recordid><startdate>20140420</startdate><enddate>20140420</enddate><creator>Takata, J</creator><creator>Li, K L</creator><creator>Leung, Gene C K</creator><creator>Kong, A K H</creator><creator>Tam, P H T</creator><creator>Hui, C Y</creator><creator>Wu, E M H</creator><creator>Xing, Yi</creator><creator>Cao, Yi</creator><creator>Tang, Sumin</creator><creator>Wang, ZhongXiang</creator><creator>Cheng, K S</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-1262-7375</orcidid><orcidid>https://orcid.org/0000-0003-1984-3852</orcidid><orcidid>https://orcid.org/0000-0002-8036-8491</orcidid><orcidid>https://orcid.org/0000-0002-6225-8918</orcidid></search><sort><creationdate>20140420</creationdate><title>MULTI-WAVELENGTH EMISSIONS FROM THE MILLISECOND PULSAR BINARY PSR J1023+0038 DURING AN ACCRETION ACTIVE STATE</title><author>Takata, J ; Li, K L ; Leung, Gene C K ; Kong, A K H ; Tam, P H T ; Hui, C Y ; Wu, E M H ; Xing, Yi ; Cao, Yi ; Tang, Sumin ; Wang, ZhongXiang ; Cheng, K S</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c454t-6cbcac67d6fce32d1f0f80a0219fb41f121dce8e85d5254920b69ffd1d0d8ea83</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>ACCRETION DISKS</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>BINARY STARS</topic><topic>COMPTON EFFECT</topic><topic>EMISSION</topic><topic>ENERGY SPECTRA</topic><topic>Fluxes</topic><topic>GAMMA RADIATION</topic><topic>Inverse</topic><topic>Millisecond pulsars</topic><topic>PULSARS</topic><topic>PULSES</topic><topic>Spectral energy distribution</topic><topic>STELLAR WINDS</topic><topic>ULTRAVIOLET RADIATION</topic><topic>WAVELENGTHS</topic><topic>X RADIATION</topic><topic>X-rays</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Takata, J</creatorcontrib><creatorcontrib>Li, K L</creatorcontrib><creatorcontrib>Leung, Gene C K</creatorcontrib><creatorcontrib>Kong, A K H</creatorcontrib><creatorcontrib>Tam, P H T</creatorcontrib><creatorcontrib>Hui, C Y</creatorcontrib><creatorcontrib>Wu, E M H</creatorcontrib><creatorcontrib>Xing, Yi</creatorcontrib><creatorcontrib>Cao, Yi</creatorcontrib><creatorcontrib>Tang, Sumin</creatorcontrib><creatorcontrib>Wang, ZhongXiang</creatorcontrib><creatorcontrib>Cheng, K S</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Takata, J</au><au>Li, K L</au><au>Leung, Gene C K</au><au>Kong, A K H</au><au>Tam, P H T</au><au>Hui, C Y</au><au>Wu, E M H</au><au>Xing, Yi</au><au>Cao, Yi</au><au>Tang, Sumin</au><au>Wang, ZhongXiang</au><au>Cheng, K S</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>MULTI-WAVELENGTH EMISSIONS FROM THE MILLISECOND PULSAR BINARY PSR J1023+0038 DURING AN ACCRETION ACTIVE STATE</atitle><jtitle>The Astrophysical journal</jtitle><date>2014-04-20</date><risdate>2014</risdate><volume>785</volume><issue>2</issue><spage>1</spage><epage>8</epage><pages>1-8</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Recent observations strongly suggest that the millisecond pulsar binary PSR J1023+0038 has developed an accretion disk since 2013 June. We present a multi-wavelength analysis of PSR J1023+0038, which reveals that (1) its gamma-rays suddenly brightened within a few days in 2013 June/July and has remained at a high gamma-ray state for several months; (2) both UV and X-ray fluxes have increased by roughly an order of magnitude; and (3) the spectral energy distribution has changed significantly after the gamma-ray sudden flux change. Time variabilities associated with UV and X-rays are on the order of 100-500 s and 50-100 s, respectively. Our model suggests that a newly formed accretion disk, due to the sudden increase of the stellar wind, could explain the changes of all these observed features. The increase of UV is emitted from the disk, and a new component in gamma-rays is produced by inverse Compton scattering between the new UV component and pulsar wind. The increase of X-rays results from the enhancement of injection pulsar wind energy into the intra-binary shock due to the increase of the stellar wind. 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| subjects | ACCRETION DISKS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY BINARY STARS COMPTON EFFECT EMISSION ENERGY SPECTRA Fluxes GAMMA RADIATION Inverse Millisecond pulsars PULSARS PULSES Spectral energy distribution STELLAR WINDS ULTRAVIOLET RADIATION WAVELENGTHS X RADIATION X-rays |
| title | MULTI-WAVELENGTH EMISSIONS FROM THE MILLISECOND PULSAR BINARY PSR J1023+0038 DURING AN ACCRETION ACTIVE STATE |
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