V373 Scuti was a nova which appeared in 1975 in the southern constellation of Scutum.[3] It was announced on June 15, 1975 by Paul Wild at the Zimmerwald Observatory, Switzerland.[7] At the time the magnitude was about 7.9.[8] The peak magnitude of 7.1 occurred a month earlier on May 11.[2]
 | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 55m 26.71s[1] |
| Declination | −07° 43′ 05.5″[1] |
| Apparent magnitude (V) | 7.1[2] (Max) – 18.7[3] |
| Details | |
| Mass | 1.02[4] M☉ |
| Rotation | 258.3 s[5] |
| Other designations | |
| Database references | |
| SIMBAD | data |
The light curve of this nova declined as a typical power law following the peak, but showed significant jittery behavior.[10] After about 40–50 days emission lines began to appear in the spectrum, which allowed measurement of the mean expansion velocity as 955±130 km/s.[8] The large amplitude flickering as well as other indicators suggest a magnetic influence, making this a candidate intermediate polar system. A luminosity modulation of 258.3 seconds is most likely due to rotation of the white dwarf.[5] The system has an orbital period of 3.69 ± 0.07 h,[3] and the light curve suggests a high orbital inclination.[5]
References
edit- ^ a b Downes, Ronald A.; et al. (June 2001), "A Catalog and Atlas of Cataclysmic Variables: The Living Edition", The Publications of the Astronomical Society of the Pacific, 113 (784): 764–768, arXiv:astro-ph/0102302, Bibcode:2001PASP..113..764D, doi:10.1086/320802, S2CID 16285959
- ^ a b Duerbeck, Hilmar W. (March 1987), "A Reference Catalogue and Atlas of Galactic Novae", Space Science Reviews, 45 (1–2): 1–14, Bibcode:1987SSRv...45....1D, doi:10.1007/BF00187826, S2CID 115854775
- ^ a b c Tappert, C.; et al. (December 2013), "Life after eruption - III. Orbital periods of the old novae V365 Car, AR Cir, V972 Oph, HS Pup, V909 Sgr, V373 Sct and CN Vel", Monthly Notices of the Royal Astronomical Society, 436 (3): 2412–2425, arXiv:1310.0394, Bibcode:2013MNRAS.436.2412T, doi:10.1093/mnras/stt1747, S2CID 118363741
- ^ Shara, Michael M.; et al. (June 2018), "The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae", The Astrophysical Journal, 860 (2): 11, arXiv:1804.06880, Bibcode:2018ApJ...860..110S, doi:10.3847/1538-4357/aabfbd, S2CID 55851634, 110
- ^ a b c d Woudt, Patrick A.; Warner, Brian (April 2003), "High-speed photometry of faint cataclysmic variables - III. V842 Cen, BY Cir, DD Cir, TV Crv, V655 CrA, CP Cru, V794 Oph, V992 Sco, EU Sct and V373 Sct", Monthly Notices of the Royal Astronomical Society, 340 (3): 1011–1019, arXiv:astro-ph/0301241, Bibcode:2003MNRAS.340.1011W, doi:10.1046/j.1365-8711.2003.06367.x, S2CID 119440496
- ^ "V373 Sct". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-06.
- ^ Wild, P. (June 1975), Gingerich, O. (ed.), "Probable Nova in Scutum", IAU Circular, 2791: 1, Bibcode:1975IAUC.2791....1W
- ^ a b c Rosino, L. (May 1978), "Spectral evolution of Nova V400 Per (1974) and Nova V373 Sct (1975)", Astrophysics and Space Science, 55 (2): 383–394, Bibcode:1978Ap&SS..55..383R, doi:10.1007/BF00642265, S2CID 121632043
- ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
- ^ Strope, Richard J.; et al. (July 2010), "Catalog of 93 Nova Light Curves: Classification and Properties", The Astronomical Journal, 140 (1): 34–62, arXiv:1004.3698, Bibcode:2010AJ....140...34S, doi:10.1088/0004-6256/140/1/34, S2CID 118537823
External links
edit- "富山市科学博物館 Toyama Science Museum". tsm.toyama.toyama.jp. Archived from the original on 2010-04-01. Retrieved 2016-12-13.