The hydrogen-burning turnoff of RS Ophiuchi (2006)

Izumi Hachisu; Mariko Kato; Seiichiro Kiyota; Katsuaki Kubotera; Hiroyuki Maehara; Kazuhiro Nakajima; Yuko Ishii; Mari Kamada; Sahori Mizoguchi; Shinji Nishiyama; Naoko Sumitomo; Ken'ichi Tanaka; Masayuki Yamanaka; Kozo Sadakane

doi:10.1086/509615

The hydrogen-burning turnoff of RS Ophiuchi (2006)

Izumi Hachisu, Mariko Kato, Seiichiro Kiyota, Katsuaki Kubotera, Hiroyuki Maehara, Kazuhiro Nakajima, Yuko Ishii, Mari Kamada, Sahori Mizoguchi, Shinji Nishiyama, Naoko Sumitomo, Ken'ichi Tanaka, Masayuki Yamanaka, Kozo Sadakane

Research output: Contribution to journal › Article › peer-review

50 Citations (Scopus)

Abstract

We report a coordinated multiband photometry of the RS Oph 2006 outburst and highlight the emission-line-free -band photometry that shows a midplateau phase y ∼ 10.2 mag from day 40 to day 75 after the discovery, followed by a sharp drop of the final decline. Such midplateau phases are observed in other two recurrent novae, U Sco and CI Aql, and are interpreted as a bright disk irradiated by the white dwarf. We have calculated theoretical light curves based on the optically thick wind theory and have reproduced the observed light curves, including the midplateau phase and the final sharp decline. This final decline is identified with the end of steady hydrogen shell burning, which turned out at about day 80. This turnoff date is consistent with the end of a supersoft X-ray phase observed with Swift. Our model suggests a white dwarf mass of 1.35 ± 0.01 M_⊙, which indicates that RS Oph is a progenitor of Type Ia supernovae. We strongly recommend the y-filter observation of novae to detect both the presence of a disk and the hydrogen burning turnoff.

Original language	English
Pages (from-to)	L141-L144
Journal	Astrophysical Journal
Volume	651
Issue number	2 II
DOIs	https://doi.org/10.1086/509615
Publication status	Published - 2006 Nov 10
Externally published	Yes

Keywords

Binaries: close
Binaries: symbiotic
Novae, cataclysmic variables
Stars: individual (RS Ophiuchi)
Supernovae: general
White dwarfs

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/509615

Cite this

@article{f5b4f0522268431587a3523363edd9ca,

title = "The hydrogen-burning turnoff of RS Ophiuchi (2006)",

abstract = "We report a coordinated multiband photometry of the RS Oph 2006 outburst and highlight the emission-line-free -band photometry that shows a midplateau phase y ∼ 10.2 mag from day 40 to day 75 after the discovery, followed by a sharp drop of the final decline. Such midplateau phases are observed in other two recurrent novae, U Sco and CI Aql, and are interpreted as a bright disk irradiated by the white dwarf. We have calculated theoretical light curves based on the optically thick wind theory and have reproduced the observed light curves, including the midplateau phase and the final sharp decline. This final decline is identified with the end of steady hydrogen shell burning, which turned out at about day 80. This turnoff date is consistent with the end of a supersoft X-ray phase observed with Swift. Our model suggests a white dwarf mass of 1.35 ± 0.01 M⊙, which indicates that RS Oph is a progenitor of Type Ia supernovae. We strongly recommend the y-filter observation of novae to detect both the presence of a disk and the hydrogen burning turnoff.",

keywords = "Binaries: close, Binaries: symbiotic, Novae, cataclysmic variables, Stars: individual (RS Ophiuchi), Supernovae: general, White dwarfs",

author = "Izumi Hachisu and Mariko Kato and Seiichiro Kiyota and Katsuaki Kubotera and Hiroyuki Maehara and Kazuhiro Nakajima and Yuko Ishii and Mari Kamada and Sahori Mizoguchi and Shinji Nishiyama and Naoko Sumitomo and Ken'ichi Tanaka and Masayuki Yamanaka and Kozo Sadakane",

note = "Funding Information: We thank the Variable Star Observing League of Japan (VSOLJ) and the American Association of Variable Star Observers (AAVSO) for the visual data of RS Oph. This research has been supported in part by Grants-in-Aid for Scientific Research (16540211, 16540219) of the Japan Society for the Promotion of Science.",

year = "2006",

month = nov,

day = "10",

doi = "10.1086/509615",

language = "English",

volume = "651",

pages = "L141--L144",

journal = "Astrophysical Journal",

issn = "0004-637X",

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number = "2 II",

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TY - JOUR

T1 - The hydrogen-burning turnoff of RS Ophiuchi (2006)

AU - Hachisu, Izumi

AU - Kato, Mariko

AU - Kiyota, Seiichiro

AU - Kubotera, Katsuaki

AU - Maehara, Hiroyuki

AU - Nakajima, Kazuhiro

AU - Ishii, Yuko

AU - Kamada, Mari

AU - Mizoguchi, Sahori

AU - Nishiyama, Shinji

AU - Sumitomo, Naoko

AU - Tanaka, Ken'ichi

AU - Yamanaka, Masayuki

AU - Sadakane, Kozo

N1 - Funding Information: We thank the Variable Star Observing League of Japan (VSOLJ) and the American Association of Variable Star Observers (AAVSO) for the visual data of RS Oph. This research has been supported in part by Grants-in-Aid for Scientific Research (16540211, 16540219) of the Japan Society for the Promotion of Science.

PY - 2006/11/10

Y1 - 2006/11/10

N2 - We report a coordinated multiband photometry of the RS Oph 2006 outburst and highlight the emission-line-free -band photometry that shows a midplateau phase y ∼ 10.2 mag from day 40 to day 75 after the discovery, followed by a sharp drop of the final decline. Such midplateau phases are observed in other two recurrent novae, U Sco and CI Aql, and are interpreted as a bright disk irradiated by the white dwarf. We have calculated theoretical light curves based on the optically thick wind theory and have reproduced the observed light curves, including the midplateau phase and the final sharp decline. This final decline is identified with the end of steady hydrogen shell burning, which turned out at about day 80. This turnoff date is consistent with the end of a supersoft X-ray phase observed with Swift. Our model suggests a white dwarf mass of 1.35 ± 0.01 M⊙, which indicates that RS Oph is a progenitor of Type Ia supernovae. We strongly recommend the y-filter observation of novae to detect both the presence of a disk and the hydrogen burning turnoff.

AB - We report a coordinated multiband photometry of the RS Oph 2006 outburst and highlight the emission-line-free -band photometry that shows a midplateau phase y ∼ 10.2 mag from day 40 to day 75 after the discovery, followed by a sharp drop of the final decline. Such midplateau phases are observed in other two recurrent novae, U Sco and CI Aql, and are interpreted as a bright disk irradiated by the white dwarf. We have calculated theoretical light curves based on the optically thick wind theory and have reproduced the observed light curves, including the midplateau phase and the final sharp decline. This final decline is identified with the end of steady hydrogen shell burning, which turned out at about day 80. This turnoff date is consistent with the end of a supersoft X-ray phase observed with Swift. Our model suggests a white dwarf mass of 1.35 ± 0.01 M⊙, which indicates that RS Oph is a progenitor of Type Ia supernovae. We strongly recommend the y-filter observation of novae to detect both the presence of a disk and the hydrogen burning turnoff.

KW - Binaries: close

KW - Binaries: symbiotic

KW - Novae, cataclysmic variables

KW - Stars: individual (RS Ophiuchi)

KW - Supernovae: general

KW - White dwarfs

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U2 - 10.1086/509615

DO - 10.1086/509615

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SN - 0004-637X

VL - 651

SP - L141-L144

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 II

ER -

The hydrogen-burning turnoff of RS Ophiuchi (2006)

Abstract

Keywords

ASJC Scopus subject areas

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