The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
- Autores
- Orio, Marina; Gendreau, Keith; Giese, Morgan; Luna, Gerardo Juan Manuel; Magdolen, Jozef; Strohmayer, Tod E.; Zhang, Andy E.; Altamirano, Diego; Dobrotka, Andrej; Enoto, Teruaki; Ferrara, Elizabeth C.; Ignace, Richard; Heinz, Sebastian; Markwardt, Craig; Nichols, Joy S.; Parker, Michael L.; Pasham, Dheeraj R.; Pei, Songpeng; Pradhan, Pragati; Remillard, Ron; Steiner, James F.; Tombesi, Francesco
- Año de publicación
- 2023
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2-12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21-25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV-500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV-2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M ⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics.
Fil: Orio, Marina. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados Unidos
Fil: Gendreau, Keith. Center for Exploration and Space Studies; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos
Fil: Giese, Morgan. University of Wisconsin; Estados Unidos
Fil: Luna, Gerardo Juan Manuel. Universidad de Buenos Aires; Argentina. Universidad Nacional de Hurlingham; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Magdolen, Jozef. Slovak University of Technology in Bratislava; Eslovaquia
Fil: Strohmayer, Tod E.. National Aeronautics and Space Administration; Estados Unidos
Fil: Zhang, Andy E.. University of Wisconsin; Estados Unidos
Fil: Altamirano, Diego. University of Southampton; Reino Unido
Fil: Dobrotka, Andrej. Slovak University of Technology in Bratislava; Eslovaquia
Fil: Enoto, Teruaki. Riken Cluster For Pioneering Research; Japón
Fil: Ferrara, Elizabeth C.. University of Maryland; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos
Fil: Ignace, Richard. East Tennessee State University; Estados Unidos
Fil: Heinz, Sebastian. University of Wisconsin; Estados Unidos
Fil: Markwardt, Craig. National Aeronautics and Space Administration; Estados Unidos
Fil: Nichols, Joy S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Parker, Michael L.. University of Cambridge; Estados Unidos
Fil: Pasham, Dheeraj R.. Mit Kavli Institute For Astrophysics And Space Research; Estados Unidos
Fil: Pei, Songpeng. Liupanshui Normal University; China
Fil: Pradhan, Pragati. Embry-riddle Aeronautical University, Prescott; China. Mit Kavli Institute For Astrophysics And Space Research; Estados Unidos
Fil: Remillard, Ron. Mit Kavli Institute For Astrophysics And Space Research; Estados Unidos
Fil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Tombesi, Francesco. University of Maryland; Estados Unidos. Universita Tor Vergata; Italia. National Aeronautics and Space Administration; Estados Unidos - Materia
-
novae
recurrent novae
high energy astrophysics
X-ray transient sources - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/220114
Ver los metadatos del registro completo
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The RS Oph Outburst of 2021 Monitored in X-Rays with NICEROrio, MarinaGendreau, KeithGiese, MorganLuna, Gerardo Juan ManuelMagdolen, JozefStrohmayer, Tod E.Zhang, Andy E.Altamirano, DiegoDobrotka, AndrejEnoto, TeruakiFerrara, Elizabeth C.Ignace, RichardHeinz, SebastianMarkwardt, CraigNichols, Joy S.Parker, Michael L.Pasham, Dheeraj R.Pei, SongpengPradhan, PragatiRemillard, RonSteiner, James F.Tombesi, Francesconovaerecurrent novaehigh energy astrophysicsX-ray transient sourceshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2-12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21-25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV-500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV-2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M ⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics.Fil: Orio, Marina. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados UnidosFil: Gendreau, Keith. Center for Exploration and Space Studies; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Giese, Morgan. University of Wisconsin; Estados UnidosFil: Luna, Gerardo Juan Manuel. Universidad de Buenos Aires; Argentina. Universidad Nacional de Hurlingham; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Magdolen, Jozef. Slovak University of Technology in Bratislava; EslovaquiaFil: Strohmayer, Tod E.. National Aeronautics and Space Administration; Estados UnidosFil: Zhang, Andy E.. University of Wisconsin; Estados UnidosFil: Altamirano, Diego. University of Southampton; Reino UnidoFil: Dobrotka, Andrej. Slovak University of Technology in Bratislava; EslovaquiaFil: Enoto, Teruaki. Riken Cluster For Pioneering Research; JapónFil: Ferrara, Elizabeth C.. University of Maryland; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Ignace, Richard. East Tennessee State University; Estados UnidosFil: Heinz, Sebastian. University of Wisconsin; Estados UnidosFil: Markwardt, Craig. National Aeronautics and Space Administration; Estados UnidosFil: Nichols, Joy S.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Parker, Michael L.. University of Cambridge; Estados UnidosFil: Pasham, Dheeraj R.. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Pei, Songpeng. Liupanshui Normal University; ChinaFil: Pradhan, Pragati. Embry-riddle Aeronautical University, Prescott; China. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Remillard, Ron. Mit Kavli Institute For Astrophysics And Space Research; Estados UnidosFil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Tombesi, Francesco. University of Maryland; Estados Unidos. Universita Tor Vergata; Italia. National Aeronautics and Space Administration; Estados UnidosIOP Publishing2023-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/220114Orio, Marina; Gendreau, Keith; Giese, Morgan; Luna, Gerardo Juan Manuel; Magdolen, Jozef; et al.; The RS Oph Outburst of 2021 Monitored in X-Rays with NICER; IOP Publishing; Astrophysical Journal; 955; 1; 9-2023; 1-260004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ace9bdinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ace9bdinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:09:33Zoai:ri.conicet.gov.ar:11336/220114instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:09:33.711CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| title |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| spellingShingle |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER Orio, Marina novae recurrent novae high energy astrophysics X-ray transient sources |
| title_short |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| title_full |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| title_fullStr |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| title_full_unstemmed |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| title_sort |
The RS Oph Outburst of 2021 Monitored in X-Rays with NICER |
| dc.creator.none.fl_str_mv |
Orio, Marina Gendreau, Keith Giese, Morgan Luna, Gerardo Juan Manuel Magdolen, Jozef Strohmayer, Tod E. Zhang, Andy E. Altamirano, Diego Dobrotka, Andrej Enoto, Teruaki Ferrara, Elizabeth C. Ignace, Richard Heinz, Sebastian Markwardt, Craig Nichols, Joy S. Parker, Michael L. Pasham, Dheeraj R. Pei, Songpeng Pradhan, Pragati Remillard, Ron Steiner, James F. Tombesi, Francesco |
| author |
Orio, Marina |
| author_facet |
Orio, Marina Gendreau, Keith Giese, Morgan Luna, Gerardo Juan Manuel Magdolen, Jozef Strohmayer, Tod E. Zhang, Andy E. Altamirano, Diego Dobrotka, Andrej Enoto, Teruaki Ferrara, Elizabeth C. Ignace, Richard Heinz, Sebastian Markwardt, Craig Nichols, Joy S. Parker, Michael L. Pasham, Dheeraj R. Pei, Songpeng Pradhan, Pragati Remillard, Ron Steiner, James F. Tombesi, Francesco |
| author_role |
author |
| author2 |
Gendreau, Keith Giese, Morgan Luna, Gerardo Juan Manuel Magdolen, Jozef Strohmayer, Tod E. Zhang, Andy E. Altamirano, Diego Dobrotka, Andrej Enoto, Teruaki Ferrara, Elizabeth C. Ignace, Richard Heinz, Sebastian Markwardt, Craig Nichols, Joy S. Parker, Michael L. Pasham, Dheeraj R. Pei, Songpeng Pradhan, Pragati Remillard, Ron Steiner, James F. Tombesi, Francesco |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
novae recurrent novae high energy astrophysics X-ray transient sources |
| topic |
novae recurrent novae high energy astrophysics X-ray transient sources |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2-12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21-25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV-500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV-2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M ⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics. Fil: Orio, Marina. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados Unidos Fil: Gendreau, Keith. Center for Exploration and Space Studies; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos Fil: Giese, Morgan. University of Wisconsin; Estados Unidos Fil: Luna, Gerardo Juan Manuel. Universidad de Buenos Aires; Argentina. Universidad Nacional de Hurlingham; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Magdolen, Jozef. Slovak University of Technology in Bratislava; Eslovaquia Fil: Strohmayer, Tod E.. National Aeronautics and Space Administration; Estados Unidos Fil: Zhang, Andy E.. University of Wisconsin; Estados Unidos Fil: Altamirano, Diego. University of Southampton; Reino Unido Fil: Dobrotka, Andrej. Slovak University of Technology in Bratislava; Eslovaquia Fil: Enoto, Teruaki. Riken Cluster For Pioneering Research; Japón Fil: Ferrara, Elizabeth C.. University of Maryland; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos Fil: Ignace, Richard. East Tennessee State University; Estados Unidos Fil: Heinz, Sebastian. University of Wisconsin; Estados Unidos Fil: Markwardt, Craig. National Aeronautics and Space Administration; Estados Unidos Fil: Nichols, Joy S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Parker, Michael L.. University of Cambridge; Estados Unidos Fil: Pasham, Dheeraj R.. Mit Kavli Institute For Astrophysics And Space Research; Estados Unidos Fil: Pei, Songpeng. Liupanshui Normal University; China Fil: Pradhan, Pragati. Embry-riddle Aeronautical University, Prescott; China. Mit Kavli Institute For Astrophysics And Space Research; Estados Unidos Fil: Remillard, Ron. Mit Kavli Institute For Astrophysics And Space Research; Estados Unidos Fil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Tombesi, Francesco. University of Maryland; Estados Unidos. Universita Tor Vergata; Italia. National Aeronautics and Space Administration; Estados Unidos |
| description |
The 2021 outburst of the symbiotic recurrent nova RS Oph was monitored with the Neutron Star Interior Composition Explorer Mission (NICER) in the 0.2-12 keV range from day one after the optical maximum, until day 88, producing an unprecedented, detailed view of the outburst development. The X-ray flux preceding the supersoft X-ray phase peaked almost 5 days after optical maximum and originated only in shocked ejecta for 21-25 days. The emission was thermal; in the first 5 days, only a non-collisional-ionization equilibrium model fits the spectrum, and a transition to equilibrium occurred between days 6 and 12. The ratio of peak X-ray flux measured in the NICER range to that measured with Fermi in the 60 MeV-500 GeV range was about 0.1, and the ratio to the peak flux measured with H.E.S.S. in the 250 GeV-2.5 TeV range was about 100. The central supersoft X-ray source (SSS), namely the shell hydrogen burning white dwarf (WD), became visible in the fourth week, initially with short flares. A huge increase in flux occurred on day 41, but the SSS flux remained variable. A quasi-periodic oscillation every ≃35 s was always observed during the SSS phase, with variations in amplitude and a period drift that appeared to decrease in the end. The SSS has characteristics of a WD of mass >1 M ⊙. Thermonuclear burning switched off shortly after day 75, earlier than in the 2006 outburst. We discuss implications for the nova physics. |
| publishDate |
2023 |
| dc.date.none.fl_str_mv |
2023-09 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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publishedVersion |
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http://hdl.handle.net/11336/220114 Orio, Marina; Gendreau, Keith; Giese, Morgan; Luna, Gerardo Juan Manuel; Magdolen, Jozef; et al.; The RS Oph Outburst of 2021 Monitored in X-Rays with NICER; IOP Publishing; Astrophysical Journal; 955; 1; 9-2023; 1-26 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/220114 |
| identifier_str_mv |
Orio, Marina; Gendreau, Keith; Giese, Morgan; Luna, Gerardo Juan Manuel; Magdolen, Jozef; et al.; The RS Oph Outburst of 2021 Monitored in X-Rays with NICER; IOP Publishing; Astrophysical Journal; 955; 1; 9-2023; 1-26 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
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eng |
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IOP Publishing |
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