SDSS J085414.02+390537.3—A New Asynchronous Polar
Based on data from the ZTF photometric survey, we have revealed asynchrony of the polar SDSS J085414.02+390537.3. A beat period days, during which the system changes its brightness by , is distinguished in the light curves. Power peaks at the white-dwarf rotation period min and orbital period min ar...
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| Veröffentlicht in: | Astronomy letters 2023-08, Vol.49 (8), p.475-485 |
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| container_title | Astronomy letters |
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| creator | Kolbin, A. I. Suslikov, M. V. Kochkina, V. Yu Borisov, N. V. Burenkov, A. N. Oparin, D. V. |
| description | Based on data from the ZTF photometric survey, we have revealed asynchrony of the polar SDSS J085414.02+390537.3. A beat period
days, during which the system changes its brightness by
, is distinguished in the light curves. Power peaks at the white-dwarf rotation period
min and orbital period
min are revealed in the periodograms, with the corresponding polar asynchrony being
. The photometric behavior of the polar points to a change of the main accreting pole during the beat period. Based on the Zeeman splitting of the H
line, we have estimated the mean magnetic field strength of the white dwarf to be
MG. The magnetic field strength near the magnetic pole has been found by modeling the cyclotron spectra to be
MG. The Doppler tomograms in the H
line exhibit a distribution of emission sources typical for polars in velocity space with evidence of the transition of the accretion stream from the ballistic trajectory to the magnetic one. |
| doi_str_mv | 10.1134/S1063773723080029 |
| format | Article |
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days, during which the system changes its brightness by
, is distinguished in the light curves. Power peaks at the white-dwarf rotation period
min and orbital period
min are revealed in the periodograms, with the corresponding polar asynchrony being
. The photometric behavior of the polar points to a change of the main accreting pole during the beat period. Based on the Zeeman splitting of the H
line, we have estimated the mean magnetic field strength of the white dwarf to be
MG. The magnetic field strength near the magnetic pole has been found by modeling the cyclotron spectra to be
MG. The Doppler tomograms in the H
line exhibit a distribution of emission sources typical for polars in velocity space with evidence of the transition of the accretion stream from the ballistic trajectory to the magnetic one.</description><identifier>ISSN: 1063-7737</identifier><identifier>EISSN: 1562-6873</identifier><identifier>DOI: 10.1134/S1063773723080029</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Astronomy ; Astrophysics and Astroparticles ; Ballistic trajectories ; Cyclotrons ; Deposition ; Field strength ; Light curve ; Magnetic fields ; Magnetic poles ; Observations and Techniques ; Orbits ; Photometry ; Physics ; Physics and Astronomy ; White dwarf stars ; Zeeman effect</subject><ispartof>Astronomy letters, 2023-08, Vol.49 (8), p.475-485</ispartof><rights>Pleiades Publishing, Inc. 2023</rights><rights>Pleiades Publishing, Inc. 2023.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c316t-141304c20d5356ad9c3fc6f6976a17492aa7ff7925e86b9bd3b9f876c2f2b5f53</citedby><cites>FETCH-LOGICAL-c316t-141304c20d5356ad9c3fc6f6976a17492aa7ff7925e86b9bd3b9f876c2f2b5f53</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1134/S1063773723080029$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1134/S1063773723080029$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids></links><search><creatorcontrib>Kolbin, A. I.</creatorcontrib><creatorcontrib>Suslikov, M. V.</creatorcontrib><creatorcontrib>Kochkina, V. Yu</creatorcontrib><creatorcontrib>Borisov, N. V.</creatorcontrib><creatorcontrib>Burenkov, A. N.</creatorcontrib><creatorcontrib>Oparin, D. V.</creatorcontrib><title>SDSS J085414.02+390537.3—A New Asynchronous Polar</title><title>Astronomy letters</title><addtitle>Astron. Lett</addtitle><description>Based on data from the ZTF photometric survey, we have revealed asynchrony of the polar SDSS J085414.02+390537.3. A beat period
days, during which the system changes its brightness by
, is distinguished in the light curves. Power peaks at the white-dwarf rotation period
min and orbital period
min are revealed in the periodograms, with the corresponding polar asynchrony being
. The photometric behavior of the polar points to a change of the main accreting pole during the beat period. Based on the Zeeman splitting of the H
line, we have estimated the mean magnetic field strength of the white dwarf to be
MG. The magnetic field strength near the magnetic pole has been found by modeling the cyclotron spectra to be
MG. The Doppler tomograms in the H
line exhibit a distribution of emission sources typical for polars in velocity space with evidence of the transition of the accretion stream from the ballistic trajectory to the magnetic one.</description><subject>Astronomy</subject><subject>Astrophysics and Astroparticles</subject><subject>Ballistic trajectories</subject><subject>Cyclotrons</subject><subject>Deposition</subject><subject>Field strength</subject><subject>Light curve</subject><subject>Magnetic fields</subject><subject>Magnetic poles</subject><subject>Observations and Techniques</subject><subject>Orbits</subject><subject>Photometry</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>White dwarf stars</subject><subject>Zeeman effect</subject><issn>1063-7737</issn><issn>1562-6873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><recordid>eNp1kM1Kw0AUhQdRsFYfwF3ApSTeOzczk1mWav2hqBBdh8kko5aa1JkG6c6H8Al9ElMiuBBX98A537lwGDtGSBApPcsRJClFihNkAFzvsBEKyWOZKdrtdW_HW3-fHYSwAABNBCNG-XmeRzeQiRTTBPgpaRCkEvr6-JxEt_V7NAmbxj77tmm7EN23S-MP2Z4zy1Af_dwxe5xdPEyv4vnd5fV0Mo8toVzHmCJBajlUgoQ0lbbkrHRSK2lQpZobo5xTmos6k6UuKyq1y5S03PFSOEFjdjL0rnz71tVhXSzazjf9y4JrFAgkBPYpHFLWtyH42hUr__Jq_KZAKLbbFH-26Rk-MKHPNk-1_23-H_oGPQJg2A</recordid><startdate>20230801</startdate><enddate>20230801</enddate><creator>Kolbin, A. I.</creator><creator>Suslikov, M. V.</creator><creator>Kochkina, V. Yu</creator><creator>Borisov, N. V.</creator><creator>Burenkov, A. N.</creator><creator>Oparin, D. V.</creator><general>Pleiades Publishing</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope></search><sort><creationdate>20230801</creationdate><title>SDSS J085414.02+390537.3—A New Asynchronous Polar</title><author>Kolbin, A. I. ; Suslikov, M. V. ; Kochkina, V. Yu ; Borisov, N. V. ; Burenkov, A. N. ; Oparin, D. V.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c316t-141304c20d5356ad9c3fc6f6976a17492aa7ff7925e86b9bd3b9f876c2f2b5f53</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Astronomy</topic><topic>Astrophysics and Astroparticles</topic><topic>Ballistic trajectories</topic><topic>Cyclotrons</topic><topic>Deposition</topic><topic>Field strength</topic><topic>Light curve</topic><topic>Magnetic fields</topic><topic>Magnetic poles</topic><topic>Observations and Techniques</topic><topic>Orbits</topic><topic>Photometry</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>White dwarf stars</topic><topic>Zeeman effect</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kolbin, A. I.</creatorcontrib><creatorcontrib>Suslikov, M. V.</creatorcontrib><creatorcontrib>Kochkina, V. Yu</creatorcontrib><creatorcontrib>Borisov, N. V.</creatorcontrib><creatorcontrib>Burenkov, A. N.</creatorcontrib><creatorcontrib>Oparin, D. V.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Kolbin, A. I.</au><au>Suslikov, M. V.</au><au>Kochkina, V. Yu</au><au>Borisov, N. V.</au><au>Burenkov, A. N.</au><au>Oparin, D. V.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>SDSS J085414.02+390537.3—A New Asynchronous Polar</atitle><jtitle>Astronomy letters</jtitle><stitle>Astron. Lett</stitle><date>2023-08-01</date><risdate>2023</risdate><volume>49</volume><issue>8</issue><spage>475</spage><epage>485</epage><pages>475-485</pages><issn>1063-7737</issn><eissn>1562-6873</eissn><abstract>Based on data from the ZTF photometric survey, we have revealed asynchrony of the polar SDSS J085414.02+390537.3. A beat period
days, during which the system changes its brightness by
, is distinguished in the light curves. Power peaks at the white-dwarf rotation period
min and orbital period
min are revealed in the periodograms, with the corresponding polar asynchrony being
. The photometric behavior of the polar points to a change of the main accreting pole during the beat period. Based on the Zeeman splitting of the H
line, we have estimated the mean magnetic field strength of the white dwarf to be
MG. The magnetic field strength near the magnetic pole has been found by modeling the cyclotron spectra to be
MG. The Doppler tomograms in the H
line exhibit a distribution of emission sources typical for polars in velocity space with evidence of the transition of the accretion stream from the ballistic trajectory to the magnetic one.</abstract><cop>Moscow</cop><pub>Pleiades Publishing</pub><doi>10.1134/S1063773723080029</doi><tpages>11</tpages></addata></record> |
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| subjects | Astronomy Astrophysics and Astroparticles Ballistic trajectories Cyclotrons Deposition Field strength Light curve Magnetic fields Magnetic poles Observations and Techniques Orbits Photometry Physics Physics and Astronomy White dwarf stars Zeeman effect |
| title | SDSS J085414.02+390537.3—A New Asynchronous Polar |
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