SN 1994D
B2000.0 | |
| Distance | 55.1 ± 5.2 Mly (16.9 ± 1.6 Mpc)[3] |
|---|---|
| Redshift | 0.0036, 0.0001, −0.0001, 0.0021, 0.0023, 0.0022, 0.0008, 0.0005, 0.0013, 0.0017, 0.0004, 0.0024, 0.0011, 0.0012, 0.0002  |
| Host | NGC 4526[2] |
| Progenitor type | White dwarf |
| Peak apparent magnitude | +15.2 |
| Preceded by | SN 1994C[4] |
| Followed by | SN 1994E[4] |
| ] | |
SN 1994D was a
″ west and 7.8″ south of the galaxy center and positioned near a prominent dust lane.[1] It was caused by the explosion of a white dwarf star composed of carbon and oxygen.[5] This event was discovered on March 7, 1994 by R. R. Treffers and associates using the automated 30-inch telescope at Leuschner Observatory.[2] It reached peak visual brightness two weeks later on March 22.[5] Modelling of the light curve indicates the explosion would have been visible around March 3-4. A possible detection of helium in the spectrum was made by W. P. S. Meikle and associates in 1996.[1] A mass of 0.014 to 0.03 M☉ in helium would be needed to produce this feature.[6]
See also
References
- ^ .
- ^ Bibcode:1994IAUC.5946....2T.
- S2CID 119430198. 104.
- ^ a b "List of Supernovae", Central Bureau for Astronomical Telegrams, International Astronomical Union, retrieved 2021-12-02.
- ^ S2CID 119535927.
- S2CID 55621728. A46.
Further reading
- Branch, David; et al. (June 2005). "Comparative Direct Analysis of Type Ia Supernova Spectra. I. SN 1994D". The Publications of the Astronomical Society of the Pacific. 117 (832): 545–552. S2CID 15250772.
External links
- Light curves and spectra Archived 2021-04-26 at the Wayback Machine on the Open Supernova Catalog Archived 2016-03-03 at the Wayback Machine
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