Статья

The Type I[CLC]c[/CLC] Hypernova SN 2002[CLC]ap[/CLC]

P. A. MazzaliDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanJ. DengDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanKeiichi MaedaDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanKen’ichi NomotoDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanHideyuki UmedaDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanK. HatanoDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanK. IwamotoDepartment of Physics, Nihon University, Chiyoda-ku, Tokyo 101-8308, JapanYuzuru YoshiiInstitute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanYukiyasu KobayashiNational Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, JapanTakeo MinezakiInstitute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanMamoru DoiInstitute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanKeigo EnyaInstitute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanHiroyuki TomitaDepartment of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanStephen SmarttInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, England, UKK. KinugasaGunma Astronomical Observatory, 6860-86 Nakayama, Takayama, Agatsuma, Gunma 377-0702, JapanHideyo KawakitaGunma Astronomical Observatory, 6860-86 Nakayama, Takayama, Agatsuma, Gunma 377-0702, JapanK. AyaniBisei Astronomical Observatory, 1723-70 Okura, Bisei, Oda, Okayama 714-1411, JapanTetsuya KawabataBisei Astronomical Observatory, 1723-70 Okura, Bisei, Oda, Okayama 714-1411, JapanH. YamaokaDepartment of Physics, School of Sciences, Kyushu University, Chuo-ku, Fukuoka 810-8560, JapanY. QiuNational Astronomical Observatories, Chinese Academy of Sciences, 20A Datsun Road, Chaoyang, Beijing 100012, ChinaKentaro MotoharaInstitute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanC. GerardyDepartment of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755-3528R. FesenDepartment of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755-3528Koji S. KawabataNational Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, JapanMasanori IyeDepartment of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo 181-8588, JapanNobunari KashikawaNational Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, JapanGeorge KosugiSubaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HW 96720Youichi OhyamaSubaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HW 96720Masahide Takada‐HidaiLiberal Arts Education Center, Tokai University, Hiratsuka, Kanagawa 259-12, JapanGang ZhaoNational Astronomical Observatories, Chinese Academy of Sciences, 20A Datsun Road, Chaoyang, Beijing 100012, ChinaR. ChornockDepartment of Astronomy, University of California at Berkeley, 601 Campbell Hall, Berkeley, CA 94720A. V. FilippenkoDepartment of Astronomy, University of California at Berkeley, 601 Campbell Hall, Berkeley, CA 94720S. BenettiINAF-Osservatorio Astronomico, Vicolo dell’Osservatorio 2, Padova I-35122, ItalyM. TurattoINAF-Osservatorio Astronomico, Vicolo dell’Osservatorio 2, Padova I-35122, Italy

2002en

ABI

Аннотация

Photometric and spectroscopic data of the energetic Type Ic supernova (SN) 2002ap are presented, and the properties of the SN are investigated through models of its spectral evolution and its light curve. The SN is spectroscopically similar to the hypernova SN 1997ef. However, its kinetic energy [~(4-10) ? 1051 ergs] and the mass ejected (2.5-5 M?) are smaller, resulting in a faster evolving light curve. The SN synthesized ~0.07 M? of 56Ni, and its peak luminosity was similar to that of normal SNe. Brightness alone should not be used to define a hypernova, whose defining character, namely very broad spectral features, is the result of high kinetic energy. The likely main-sequence mass of the progenitor star was 20-25 M?, which is also lower than that of both hypernovae SN 1997ef and SN 1998bw. SN 2002ap appears to lie at the low-energy and low-mass end of the hypernova sequence as it is known so far. Observations of the nebular spectrum, which is expected to dominate by the summer of 2002, are necessary to confirm these values.

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Идентификаторы

DOI: 10.1086/341504

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Цитирований: 2Использованных источников: 0

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