دورية أكاديمية
A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?
| العنوان: | A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if? |
|---|---|
| المؤلفون: | Zhang JJ(张居甲), Wang, Xiao-Feng, Sasdelli, Michele, Zhang, Tian-Meng, Liu, Zheng-Wei, Mazzali, Paolo A., Meng XC(孟祥存), Maeda, Keiichi, Chen, Jun-Cheng, Huang, Fang, Zhao, Xu-Lin, Zhang, Kai-Cheng, Zhai Q(翟倩), Pian, Elena, Wang B(王博), Chang L(常亮), Yi WM(易卫敏), Wang CJ(王传军), Wang XL(王雪利), Xin YX(辛玉新), Wang JG(王建国), Lun BL(伦宝利), Zheng XM(郑向明), Zhang XL(张西亮), Fan YF(范玉峰), Bai JM(白金明) |
| بيانات النشر: | IOP PUBLISHING LTD |
| سنة النشر: | 2016 |
| المجموعة: | Yunnan Observatories: YNAO OpenIR (Chinese Academy of Sciences, CAS) / 中国科学院云南天文台机构知识库 |
| مصطلحات موضوعية: | galaxies: individual (NGC 2691), supernovae: general, supernovae: individual (SN 2011hr, SN 1991T, SN 2007if), 天文学, 天文学::星系与宇宙学, 天文学::星系与宇宙学::星系天文学, 天文学::恒星与银河系, 天文学::恒星与银河系::恒星天文学, 理学, 理学::天文学, Astronomy & Astrophysics, GRAVITATIONALLY CONFINED DETONATION, NEAR-INFRARED OBSERVATIONS, HIGH-VELOCITY FEATURES, HUBBLE-SPACE-TELESCOPE, LIGHT CURVES, ABUNDANCE STRATIFICATION, WHITE-DWARF, SPECTROSCOPIC OBSERVATIONS, ULTRAVIOLET OBSERVATIONS, EXPLOSION, Science & Technology, Physical Sciences |
| الوصف: | Photometric and spectroscopic observations of a slowly declining, luminous Type Ia supernova (SN Ia) SN 2011hr in the starburst galaxy NGC 2691 are presented. SN. 2011hr is found to peak at MB = -19.84 +/- 0.40 mag, with a postmaximum decline rate Delta(m15)(B) = 0.92. +/- 0.03 mag. From the maximum-light bolometric luminosity, L = (2.30 +/- 0.90) x 10(43) erg s(-1), we estimate the mass of synthesized Ni-56 in SN 2011hr to be M(Ni-56) = 1.11 +/- 0.43M(circle dot). SN 2011hr appears more luminous than SN 1991T at around maximum light, and the absorption features from its intermediate-mass elements (IMEs) are noticeably weaker than those of the latter at similar phases. Spectral modeling suggests that SN 2011hr has IMEs of similar to 0.07 M-circle dot in the outer ejecta, which is much lower than the typical value of normal SNe Ia (i.e., 0.3-0.4 M-circle dot) and is also lower than the value of SN 1991T (i.e., similar to 0.18 M-circle dot). These results indicate that SN. 2011hr may arise from a Chandrasekhar-mass white dwarf progenitor that experienced a more efficient burning process in the explosion. Nevertheless, it is still possible that SN. 2011hr may serve as a transitional object connecting the SN 1991T-like SNe Ia with a superluminous subclass like SN 2007if given that the latter also shows very weak IMEs at all phases. |
| نوع الوثيقة: | article in journal/newspaper report |
| اللغة: | English |
| العلاقة: | ASTROPHYSICAL JOURNAL; http://ir.ynao.ac.cn/handle/114a53/9337Test; http://iopscience.iop.org/article/10.3847/0004-637X/817/2/114/metaTest |
| DOI: | 10.3847/0004-637X/817/2/114/meta |
| DOI: | 10.3847/0004-637X/817/2/114 |
| الإتاحة: | https://doi.org/10.3847/0004-637X/817/2/114Test http://ir.ynao.ac.cn/handle/114a53/9337Test |
| رقم الانضمام: | edsbas.D3323CD7 |
| قاعدة البيانات: | BASE |
| DOI: | 10.3847/0004-637X/817/2/114/meta |
|---|