The Remarkable Spin-down and Ultrafast Outflows of the Highly Pulsed Supersoft Source of Nova Herculis 2021
Nova Her 2021 (V1674 Her), which erupted on 2021 June 12, reached naked-eye brightness and has been detected from radio to γ -rays. An extremely fast optical decline of 2 magnitudes in 1.2 days and strong Ne lines imply a high-mass white dwarf. The optical pre-outburst detection of a 501.42 s oscill...
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| Veröffentlicht in: | Astrophysical journal. Letters 2021-12, Vol.922 (2), p.L42 |
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| creator | Drake, Jeremy J. Ness, Jan-Uwe Page, Kim L. Luna, G. J. M. Beardmore, Andrew P. Orio, Marina Osborne, Julian P. Mróz, Przemek Starrfield, Sumner Banerjee, Dipankar P. K. Balman, Solen Darnley, M. J. Bhargava, Y. Dewangan, G. C. Singh, K. P. |
| description | Nova Her 2021 (V1674 Her), which erupted on 2021 June 12, reached naked-eye brightness and has been detected from radio to
γ
-rays. An extremely fast optical decline of 2 magnitudes in 1.2 days and strong Ne lines imply a high-mass white dwarf. The optical pre-outburst detection of a 501.42 s oscillation suggests a magnetic white dwarf. This is the first time that an oscillation of this magnitude has been detected in a classical nova prior to outburst. We report X-ray outburst observations from Swift and Chandra that uniquely show (1) a very strong modulation of supersoft X-rays at a different period from reported optical periods, (2) strong pulse profile variations and the possible presence of period variations of the order of 0.1–0.3 s, and (3) rich grating spectra that vary with modulation phase and show P Cygni–type emission lines with two dominant blueshifted absorption components at ∼3000 and 9000 km s
−1
indicating expansion velocities up to 11,000 km s
−1
. X-ray oscillations most likely arise from inhomogeneous photospheric emission related to the magnetic field. Period differences between reported pre- and post-outburst optical observations, if not due to other period drift mechanisms, suggest a large ejected mass for such a fast nova, in the range 2 × 10
−5
–2 × 10
−4
M
⊙
. A difference between the period found in the Chandra data and a reported contemporaneous post-outburst optical period, as well as the presence of period drifts, could be due to weakly nonrigid photospheric rotation. |
| doi_str_mv | 10.3847/2041-8213/ac34fd |
| format | Article |
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γ
-rays. An extremely fast optical decline of 2 magnitudes in 1.2 days and strong Ne lines imply a high-mass white dwarf. The optical pre-outburst detection of a 501.42 s oscillation suggests a magnetic white dwarf. This is the first time that an oscillation of this magnitude has been detected in a classical nova prior to outburst. We report X-ray outburst observations from Swift and Chandra that uniquely show (1) a very strong modulation of supersoft X-rays at a different period from reported optical periods, (2) strong pulse profile variations and the possible presence of period variations of the order of 0.1–0.3 s, and (3) rich grating spectra that vary with modulation phase and show P Cygni–type emission lines with two dominant blueshifted absorption components at ∼3000 and 9000 km s
−1
indicating expansion velocities up to 11,000 km s
−1
. X-ray oscillations most likely arise from inhomogeneous photospheric emission related to the magnetic field. Period differences between reported pre- and post-outburst optical observations, if not due to other period drift mechanisms, suggest a large ejected mass for such a fast nova, in the range 2 × 10
−5
–2 × 10
−4
M
⊙
. A difference between the period found in the Chandra data and a reported contemporaneous post-outburst optical period, as well as the presence of period drifts, could be due to weakly nonrigid photospheric rotation.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/ac34fd</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>Cataclysmic variable stars ; Classical novae ; DQ Herculis stars ; Dwarf novae ; Emission ; Emission lines ; Fast novae ; Gamma rays ; Magnetic fields ; Modulation ; Novae ; Optical observations ; Photosphere ; Stellar winds ; White dwarf stars ; X-ray astronomy ; X-ray novae ; X-ray transient sources ; X-rays</subject><ispartof>Astrophysical journal. Letters, 2021-12, Vol.922 (2), p.L42</ispartof><rights>2021. The Author(s). Published by the American Astronomical Society.</rights><rights>Copyright IOP Publishing Dec 01, 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c381t-c62e6b23601803bc1919cded1fb01d3090576e291416aaf54e800186c3eab38d3</citedby><cites>FETCH-LOGICAL-c381t-c62e6b23601803bc1919cded1fb01d3090576e291416aaf54e800186c3eab38d3</cites><orcidid>0000-0002-1359-6312 ; 0000-0003-0156-3377 ; 0000-0003-1589-2075 ; 0000-0003-1563-9803 ; 0000-0001-6135-1144 ; 0000-0002-0210-2276 ; 0000-0001-5624-2613 ; 0000-0002-1041-7542 ; 0000-0002-2647-4373 ; 0000-0001-5186-5950 ; 0000-0003-4896-2543 ; 0000-0001-6952-3887 ; 0000-0002-5967-8399 ; 0000-0001-7016-1692 ; 0000-0003-0440-7193</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/ac34fd/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,777,781,27905,27906,38849,38871,53821,53848</link.rule.ids></links><search><creatorcontrib>Drake, Jeremy J.</creatorcontrib><creatorcontrib>Ness, Jan-Uwe</creatorcontrib><creatorcontrib>Page, Kim L.</creatorcontrib><creatorcontrib>Luna, G. J. M.</creatorcontrib><creatorcontrib>Beardmore, Andrew P.</creatorcontrib><creatorcontrib>Orio, Marina</creatorcontrib><creatorcontrib>Osborne, Julian P.</creatorcontrib><creatorcontrib>Mróz, Przemek</creatorcontrib><creatorcontrib>Starrfield, Sumner</creatorcontrib><creatorcontrib>Banerjee, Dipankar P. K.</creatorcontrib><creatorcontrib>Balman, Solen</creatorcontrib><creatorcontrib>Darnley, M. J.</creatorcontrib><creatorcontrib>Bhargava, Y.</creatorcontrib><creatorcontrib>Dewangan, G. C.</creatorcontrib><creatorcontrib>Singh, K. P.</creatorcontrib><title>The Remarkable Spin-down and Ultrafast Outflows of the Highly Pulsed Supersoft Source of Nova Herculis 2021</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>Nova Her 2021 (V1674 Her), which erupted on 2021 June 12, reached naked-eye brightness and has been detected from radio to
γ
-rays. An extremely fast optical decline of 2 magnitudes in 1.2 days and strong Ne lines imply a high-mass white dwarf. The optical pre-outburst detection of a 501.42 s oscillation suggests a magnetic white dwarf. This is the first time that an oscillation of this magnitude has been detected in a classical nova prior to outburst. We report X-ray outburst observations from Swift and Chandra that uniquely show (1) a very strong modulation of supersoft X-rays at a different period from reported optical periods, (2) strong pulse profile variations and the possible presence of period variations of the order of 0.1–0.3 s, and (3) rich grating spectra that vary with modulation phase and show P Cygni–type emission lines with two dominant blueshifted absorption components at ∼3000 and 9000 km s
−1
indicating expansion velocities up to 11,000 km s
−1
. X-ray oscillations most likely arise from inhomogeneous photospheric emission related to the magnetic field. Period differences between reported pre- and post-outburst optical observations, if not due to other period drift mechanisms, suggest a large ejected mass for such a fast nova, in the range 2 × 10
−5
–2 × 10
−4
M
⊙
. A difference between the period found in the Chandra data and a reported contemporaneous post-outburst optical period, as well as the presence of period drifts, could be due to weakly nonrigid photospheric rotation.</description><subject>Cataclysmic variable stars</subject><subject>Classical novae</subject><subject>DQ Herculis stars</subject><subject>Dwarf novae</subject><subject>Emission</subject><subject>Emission lines</subject><subject>Fast novae</subject><subject>Gamma rays</subject><subject>Magnetic fields</subject><subject>Modulation</subject><subject>Novae</subject><subject>Optical observations</subject><subject>Photosphere</subject><subject>Stellar winds</subject><subject>White dwarf stars</subject><subject>X-ray astronomy</subject><subject>X-ray novae</subject><subject>X-ray transient sources</subject><subject>X-rays</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><recordid>eNp1kM1LwzAYh4MoOKd3jwHBk3X56LL0KEOdMJy47RzSfLhutalJ69h_b0pFL3rKS3h-v_flAeASo1vK08mIoBQnnGA6koqmVh-Bwc_X8c-MxqfgLIQtQgQxzAdgt9oY-Grepd_JvDRwWRdVot2-grLScF02XloZGrhoG1u6fYDOwiZGZsXbpjzAl7YMRsNlWxsfnG3g0rVemY56dp8SzoxXbVkESBDB5-DEyshffL9DsH64X01nyXzx-DS9myeKctwkihHDckIZwhzRXOEMZ0objW2OsKYoQ-MJMyTDKWZS2nFqOIooU9TInHJNh-Cq7629-2hNaMQ2XlXFlYIwNKE045RFCvWU8i4Eb6yofRE9HARGolMqOmei8yd6pTFy3UcKV_92ynpbiowQQcQ8JaLWNoI3f4D_9n4B9HeEDw</recordid><startdate>20211201</startdate><enddate>20211201</enddate><creator>Drake, Jeremy J.</creator><creator>Ness, Jan-Uwe</creator><creator>Page, Kim L.</creator><creator>Luna, G. J. M.</creator><creator>Beardmore, Andrew P.</creator><creator>Orio, Marina</creator><creator>Osborne, Julian P.</creator><creator>Mróz, Przemek</creator><creator>Starrfield, Sumner</creator><creator>Banerjee, Dipankar P. K.</creator><creator>Balman, Solen</creator><creator>Darnley, M. J.</creator><creator>Bhargava, Y.</creator><creator>Dewangan, G. C.</creator><creator>Singh, K. P.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-1359-6312</orcidid><orcidid>https://orcid.org/0000-0003-0156-3377</orcidid><orcidid>https://orcid.org/0000-0003-1589-2075</orcidid><orcidid>https://orcid.org/0000-0003-1563-9803</orcidid><orcidid>https://orcid.org/0000-0001-6135-1144</orcidid><orcidid>https://orcid.org/0000-0002-0210-2276</orcidid><orcidid>https://orcid.org/0000-0001-5624-2613</orcidid><orcidid>https://orcid.org/0000-0002-1041-7542</orcidid><orcidid>https://orcid.org/0000-0002-2647-4373</orcidid><orcidid>https://orcid.org/0000-0001-5186-5950</orcidid><orcidid>https://orcid.org/0000-0003-4896-2543</orcidid><orcidid>https://orcid.org/0000-0001-6952-3887</orcidid><orcidid>https://orcid.org/0000-0002-5967-8399</orcidid><orcidid>https://orcid.org/0000-0001-7016-1692</orcidid><orcidid>https://orcid.org/0000-0003-0440-7193</orcidid></search><sort><creationdate>20211201</creationdate><title>The Remarkable Spin-down and Ultrafast Outflows of the Highly Pulsed Supersoft Source of Nova Herculis 2021</title><author>Drake, Jeremy J. ; Ness, Jan-Uwe ; Page, Kim L. ; Luna, G. J. M. ; Beardmore, Andrew P. ; Orio, Marina ; Osborne, Julian P. ; Mróz, Przemek ; Starrfield, Sumner ; Banerjee, Dipankar P. K. ; Balman, Solen ; Darnley, M. J. ; Bhargava, Y. ; Dewangan, G. C. ; Singh, K. 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P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Remarkable Spin-down and Ultrafast Outflows of the Highly Pulsed Supersoft Source of Nova Herculis 2021</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2021-12-01</date><risdate>2021</risdate><volume>922</volume><issue>2</issue><spage>L42</spage><pages>L42-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>Nova Her 2021 (V1674 Her), which erupted on 2021 June 12, reached naked-eye brightness and has been detected from radio to
γ
-rays. An extremely fast optical decline of 2 magnitudes in 1.2 days and strong Ne lines imply a high-mass white dwarf. The optical pre-outburst detection of a 501.42 s oscillation suggests a magnetic white dwarf. This is the first time that an oscillation of this magnitude has been detected in a classical nova prior to outburst. We report X-ray outburst observations from Swift and Chandra that uniquely show (1) a very strong modulation of supersoft X-rays at a different period from reported optical periods, (2) strong pulse profile variations and the possible presence of period variations of the order of 0.1–0.3 s, and (3) rich grating spectra that vary with modulation phase and show P Cygni–type emission lines with two dominant blueshifted absorption components at ∼3000 and 9000 km s
−1
indicating expansion velocities up to 11,000 km s
−1
. X-ray oscillations most likely arise from inhomogeneous photospheric emission related to the magnetic field. Period differences between reported pre- and post-outburst optical observations, if not due to other period drift mechanisms, suggest a large ejected mass for such a fast nova, in the range 2 × 10
−5
–2 × 10
−4
M
⊙
. A difference between the period found in the Chandra data and a reported contemporaneous post-outburst optical period, as well as the presence of period drifts, could be due to weakly nonrigid photospheric rotation.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/ac34fd</doi><tpages>9</tpages><orcidid>https://orcid.org/0000-0002-1359-6312</orcidid><orcidid>https://orcid.org/0000-0003-0156-3377</orcidid><orcidid>https://orcid.org/0000-0003-1589-2075</orcidid><orcidid>https://orcid.org/0000-0003-1563-9803</orcidid><orcidid>https://orcid.org/0000-0001-6135-1144</orcidid><orcidid>https://orcid.org/0000-0002-0210-2276</orcidid><orcidid>https://orcid.org/0000-0001-5624-2613</orcidid><orcidid>https://orcid.org/0000-0002-1041-7542</orcidid><orcidid>https://orcid.org/0000-0002-2647-4373</orcidid><orcidid>https://orcid.org/0000-0001-5186-5950</orcidid><orcidid>https://orcid.org/0000-0003-4896-2543</orcidid><orcidid>https://orcid.org/0000-0001-6952-3887</orcidid><orcidid>https://orcid.org/0000-0002-5967-8399</orcidid><orcidid>https://orcid.org/0000-0001-7016-1692</orcidid><orcidid>https://orcid.org/0000-0003-0440-7193</orcidid><oa>free_for_read</oa></addata></record> |
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| source | IOP Publishing Free Content; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; IOPscience extra; Alma/SFX Local Collection |
| subjects | Cataclysmic variable stars Classical novae DQ Herculis stars Dwarf novae Emission Emission lines Fast novae Gamma rays Magnetic fields Modulation Novae Optical observations Photosphere Stellar winds White dwarf stars X-ray astronomy X-ray novae X-ray transient sources X-rays |
| title | The Remarkable Spin-down and Ultrafast Outflows of the Highly Pulsed Supersoft Source of Nova Herculis 2021 |
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