Статья

Observations of the very young Type Ia Supernova 2019np with early-excess emission

Hanna SaiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, ChinaXiaofeng WangBeijing Planetarium, Beijing Academy of Science and Technology , Beijing 100044, ChinaN. Elias–RosaINAF – Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyYi YangDepartment of Astronomy, University of California , Berkeley, CA 94720-3411, USAJujia ZhangCenter for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100012, ChinaWeili LinPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, ChinaJun MoPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, ChinaAnthony L. PiroCarnegie Observatories , 813 Santa Barbara Street, Pasadena, CA 91101, USAXiangyun ZengCenter for Astronomy and Space Sciences, China Three Gorges University , Yichang 443000, ChinaA. ReguittiDepartamento de Ciencias Físicas – Universidad Andrés Bello , Avda. República 252, Santiago 8320000, ChilePeter J. BrownGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy, Texas A. & M. University , 4242 TAMU, College Station, TX 77843, USAChris R. BurnsCarnegie Observatories , 813 Santa Barbara Street, Pasadena, CA 91101, USAYongzhi CaiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, ChinaA. FioreINAF – Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyE. Y. HsiaoDepartment of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USAJ. IsernDepartment of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USAKiyoshi ItagakiWenxiong LiThe School of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, IsraelZhitong LiKey Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, ChinaP. J. PessiFacultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, La Plata, B1900FWA, Buenos Aires, ArgentinaM. M. PhillipsCarnegie Observatories, Las Campanas Observatory , Colina El Pino, Casilla 601, ChileS. SchuldtMax-Planck-Institut für Astrophysik , Karl-Schwarzschild Str 1, D-85741 Garching, GermanyMelissa ShahbandehDepartment of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USAM. StritzingerDepartment of Physics and Astronomy, Aarhus University , Ny Munkegade 120, DK-8000 Aarhus C, DenmarkL. TomasellaINAF – Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyC. VoglMax-Planck-Institut für Astrophysik , Karl-Schwarzschild Str 1, D-85741 Garching, GermanyBo WangYunnan Observatories (YNAO), Chinese Academy of Sciences , Kunming 650216, ChinaLingzhi WangCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaChengyuan WuPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, ChinaS. YangDepartment of Astronomy, The Oskar Klein Center, Stockholm University , AlbaNova, SE-10691 Stockholm, SwedenJicheng ZhangCenter for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100012, ChinaTianmeng ZhangKey Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, ChinaXinghan ZhangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University , Beijing 100084, China

2022en

ABI

Аннотация

ABSTRACT Early-time radiative signals from Type Ia supernovae (SNe Ia) can provide important constraints on the explosion mechanism and the progenitor system. We present observations and analysis of SN 2019np, a nearby SN Ia discovered within 1–2 days after the explosion. Follow-up observations were conducted in optical, ultraviolet, and near-infrared bands, covering the phases from ∼−16.7 d to ∼+ 367.8 d relative to its B-band peak luminosity. The photometric and spectral evolutions of SN 2019np resemble the average behaviour of normal SNe Ia. The absolute B-band peak magnitude and the post-peak decline rate are Mmax(B) = −19.52 ± 0.47 mag and Δm15(B) = 1.04 ± 0.04 mag, respectively. No Hydrogen line has been detected in the nebular-phase spectra of SN 2019np. Assuming that the 56Ni powering the light curve is centrally located, we find that the bolometric light curve of SN 2019np shows a flux excess up to 5.0 per cent in the early phase compared to the radiative diffusion model. Such an extra radiation perhaps suggests the presence of an additional energy source beyond the radioactive decay of central nickel. Comparing the observed colour evolution with that predicted by different models, such as interactions of SN ejecta with circumstellar matter (CSM)/companion star, a double-detonation explosion from a sub-Chandrasekhar mass white dwarf (WD) and surface 56Ni mixing, we propose that the nickel mixing is more favoured for SN 2019np.

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Идентификаторы

DOI: 10.1093/mnras/stac1525

Цитирования и источники

Цитирований: 2Использованных источников: 0

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