Astronomy:SN 2019np
| Event type | Supernova |
|---|---|
| Spectral class | Type Ia[1] |
| Constellation | Leo Minor |
| Right ascension | 10h 29m 21.980s[2] |
| Declination | +29° 30′ 38.30″[2] |
| Epoch | J2000 |
| Distance | 107.0 ± 22.2 Mly (32.80 ± 6.8 Mpc)[3] |
| Redshift | 0.00452[2] |
| Host | NGC 3254[2] |
| Colour (B-V) | −0.06±0.03[3] |
| Peak apparent magnitude | 13.62±0.15[3] |
SN 2019np was a Type Ia supernova[1] event in NGC 3254, which is an unbarred spiral galaxy in the northern Constellation of Leo Minor. Based on the Tully–Fisher relation, this galaxy is located at a distance of 107.0 ± 22.2 million light-years (32.80 ± 6.8 Mpc) from the Milky Way.[3] This supernova was discovered January 9, 2019 by Kōichi Itagaki,[2] and reached maximum two weeks later.[4] It was the brightest supernova observed in the year 2019.[5]
Observations
This supernova was discovered by Japanese amateur astronomer Kōichi Itagaki on January 9, 2019, using a 0.35-m telescope.[2] The early spectrum was consistent with a Type Ia supernova.[1][6] On January 11, it was measured at an apparent visual magnitude of 16.68 with an estimated two weeks until maximum.[4] It reached visual magnitude 13.6 at maximum.[3]
The spectral evolution of SN 2019np followed the normal pattern for a Type Ia supernova. The velocity of the ejecta was around 10,200 km/s at maximum, as measured from ionized silicon. Early observations showed an infrared excess, which may be explained by a collision between the ejecta and a companion star. The data is best explained by a solar mass companion on the main sequence.[3]
The explosion data is most consistent with a carbon-oxygen white dwarf that evolved from a star with five times the mass of the Sun. This compact object accreted matter from its companion until its mass approached the Chandrasekhar limit, when it detonated.[7] The explosion generated an estimated 0.66±0.05 M☉ of synthesized nickel.[3]
References
- ↑ 1.0 1.1 1.2 Wu, Chengyuan (January 2019), "Spectroscopic Classification of AT 2019np as a Young Type Ia Supernova", The Astronomer's Telegram 12374, Bibcode: 2019ATel12374....1W.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 "SN 2019np", Transient Name Server (IAU Supernova Working Group), https://www.wis-tns.org/object/2019np, retrieved 2026-03-21.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Sai, Hanna (August 2022), "Observations of the very young Type Ia Supernova 2019np with early-excess emission", Monthly Notices of the Royal Astronomical Society 514 (3): 3541–3558, doi:10.1093/mnras/stac1525, Bibcode: 2022MNRAS.514.3541S.
- ↑ 4.0 4.1 Konyves-Toth, R. (January 2019), "BVRI Photometry of the Young Type Ia SN 2019np", The Astronomer's Telegram 12378, Bibcode: 2019ATel12378....1K.
- ↑ Bishop, David, Bright Supernovae - 2019, https://www.rochesterastronomy.org/sn2019/index.html, retrieved 2024-12-09.
- ↑ Kilpatrick, C. D.; Foley, R. J. (January 2019), "Spectroscopic Classification of AT2019np with Faulkes-North/FLOYDS", The Astronomer's Telegram 12375, Bibcode: 2019ATel12375....1K.
- ↑ Hoeflich, Peter (March 2023), "The core normal Type Ia supernova 2019np - an overall spherical explosion with an aspherical surface layer and an aspherical 56Ni core", Monthly Notices of the Royal Astronomical Society 520 (1): 560–582, doi:10.1093/mnras/stad172, Bibcode: 2023MNRAS.520..560H.
Further reading
- Perez-Torres, M. (January 2019), "Radio constraints on the mass-loss rate of the Type Ia SN 2019np", The Astronomer's Telegram 12411, Bibcode: 2019ATel12411....1P.
- Konyves-Toth, R. (January 2019), "BVRI Photometry of the Young Type Ia SN 2019np", The Astronomer's Telegram 12378, Bibcode: 2019ATel12378....1K.
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