Статья

The UV/optical spectra of the Type Ia supernova SN 2010jn: a bright supernova with outer layers rich in iron-group elements

Stephan HachingerMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, GermanyP. A. MazzaliIstituto Nazionale di Astrofisica-OAPd, vicolo dell'Osservatorio 5, I-35122 Padova, ItalyM. SullivanDepartment of Physics (Astrophysics), University of Oxford, Keble Road, Oxford OX1 3RHRichard S. EllisCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAK. MaguireDepartment of Physics (Astrophysics), University of Oxford, Keble Road, Oxford OX1 3RHA. Gal‐YamBenoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, IsraelD. A. HowellLas Cumbres Observatory Global Telescope Network, Goleta, CA 93117, USAP. NugentComputational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley CA 94720, USAE. BaronHomer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W Brooks, Norman, OK 73019, USAJeff CookeCentre for Astrophysics & Supercomputing, Swinburne University of Technology, Mail H30, PO Box 218, Hawthorn, Victoria 3122, AustraliaI. ArcaviBenoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, IsraelD. BersierAstrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LDB. DildayLas Cumbres Observatory Global Telescope Network, Goleta, CA 93117, USAP. A. JamesAstrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LDM. M. KasliwalObservatories of the Carnegie Institution of Science, 813 Santa Barbara St, Pasadena, CA 91101, USAS. R. KulkarniCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAE. O. OfekBenoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, IsraelRuss R. LaherSpitzer Science Center, California Institute of Technology, M/S 314-6, Pasadena, CA 91125, USAJ. Parrent6127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755, USAJ. SuraceSpitzer Science Center, California Institute of Technology, M/S 314-6, Pasadena, CA 91125, USAO. YaronBenoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, IsraelE. S. WalkerScuola Normale Superiore di Pisa, Piazza dei Cavalieri 7, I-56126 Pisa, Italy

2013en

ABI

Аннотация

Radiative transfer studies of Type Ia supernovae (SNe Ia) hold the promise of constraining both the density profile of the SN ejecta and its stratification by element abundance which, in turn, may discriminate between different explosion mechanisms and progenitor classes. Here we analyse the Type Ia SN 2010jn (PTF10ygu) in detail, presenting and evaluating near-ultraviolet (near-UV) spectra from the Hubble Space Telescope and ground-based optical spectra and light curves. SN 2010jn was discovered by the Palomar Transient Factory (PTF) 15 d before maximum light, allowing us to secure a time series of four near-UV spectra at epochs from −10.5 to +4.8 d relative to B-band maximum. The photospheric near-UV spectra are excellent diagnostics of the iron-group abundances in the outer layers of the ejecta, particularly those at very early times. Using the method of ‘Abundance Tomography’ we derive iron-group abundances in SN 2010jn with a precision better than in any previously studied SN Ia. Optimum fits to the data can be obtained if burned material is present even at high velocities, including significant mass fractions of iron-group elements. This is consistent with the slow decline rate (or high ‘stretch’) of the light curve of SN 2010jn, and consistent with the results of delayed-detonation models. Early-phase UV spectra and detailed time-dependent series of further SNe Ia offer a promising probe of the nature of the SN Ia mechanism.

Перевод пока недоступен

Идентификаторы

DOI: 10.1093/mnras/sts492

Цитирования и источники

Цитирований: 3Использованных источников: 0

Показатели — AkademScholar · Скоро