Optical and Near-Infrared Photometry of Nova V2362 Cyg: Rebrightening Event and Dust Formation

被引：8

作者：

Arai, Akira ^{[1
]}

Uemura, Makoto ^{[2
]}

Kawabata, Koji S. ^{[2
]}

Maehara, Hiroyuki ^{[3
]}

Nakajima, Kazuhiro ^{[4
]}

Kiyota, Seiichiro ^{[5
]}

Kato, Taichi ^{[6
]}

Ohsugi, Takashi ^{[1
,2
]}

Yamashita, Takuya ^{[2
]}

Isogai, Mizuki ^{[1
]}

Nagae, Osamu ^{[1
]}

Chiynobu, Shingo ^{[1
]}

Fukazawa, Yasushi ^{[1
]}

Mizuno, Tsunefumi ^{[1
]}

Katagiri, Hideaki ^{[1
]}

Takahashi, Hiromitsu ^{[2
]}

Okita, Kiichi ^{[7
]}

Yoshida, Michitoshi ^{[7
]}

Yanagisawa, Kenshi ^{[7
]}

Sato, Shuji ^{[8
]}

Kino, Masaru ^{[8
]}

Kitagawa, Masahiro ^{[8
]}

Sadakane, Kozo ^{[9
]}

机构：

[1] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[2] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

[3] Kyoto Univ, Kuwasan Observ, Yamashina Ku, Kyoto 6078471, Japan

[4] VSOLJ, Kumano, Mie 5194673, Japan

[5] VSOLJ, Tsukuba, Ibaraki 3050031, Japan

[6] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan

[7] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan

[8] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan

[9] Osaka Kyoiku Univ, Astron Inst, Osaka 5828582, Japan

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN | 2010年 / 62卷 / 04期

关键词：

infrared: stars; ISM:; dust; extinction; stars: individual (V2362 Cyg); stars:; novae; cataclysmic variables; V2491; CYGNI; EVOLUTION; RADIATION; EMISSION;

D O I：

10.1093/pasj/62.4.1103

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present optical and near-infrared (NIR) photometry of a classical nova, V2362 Cyg (= Nova Cygni 2006). V2362 Cyg experienced a peculiar rebrightening during the period between 100 and 240d after the maximum of the nova. Our multicolor observation indicates the emergence of a pseudophotosphere with an effective temperature of similar to 9000 K at the rebrightening maximum. After the rebrightening maximum, the object showed a slow fading homogeneously in all of the used bands for one week. This implies that the fading soon after the rebrightening maximum (less than or similar to 1 week) was caused by a slowly shrinking pseudophotosphere. Then, the NIR flux drastically increased, while the optical flux steeply declined. The optical and NIR fluxes were consistent with blackbody radiation with a temperature of similar to 1500 K during this NIR rising phase. These facts are likely to be explained by dust formation in the nova ejecta. Assuming an optically thin case, we estimated the dust mass to be 10(-10)-10(-8) M-circle dot, which is less than those in typical dust-forming novae. These results support the senario that a second, long-lasting outflow which caused the rebrightening interacted with a fraction of the initial outflow and formed dust grains.

引用

页码：1103 / 1108

页数：6

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