// Workers AI · dad joke modeWhat did DM Geminorum say to its twin star? "Gem-in" me a break.
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| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Gemini |
| Right ascension | 06h 44m 12.05s[1] |
| Declination | +29° 56′ 41.9″[1] |
| Apparent magnitude (V) | 4.8v — 16.7p[1] |
| Characteristics | |
| Variable type | Classical Nova, Intermediate polar? |
| Other designations | |
| Nova Gem 1903, DM Gem, HD 48328, AAVSO 0637+30, HR 2472 | |
| Database references | |
| SIMBAD | data |
DM Geminorum also known as Nova Geminorum 1903 was a nova which erupted in the constellation Gemini in 1903. It was discovered by Herbert Hall Turner at the Greenwich Observatory on a Carte du Ciel photographic plate taken on 16 March 1903. Post-discovery examination of earlier photographs of the region taken at the Harvard College Observatory showed that the star was fainter than apparent magnitude 9 on 2 March 1903, and magnitude 5.1 on 6 March 1903, making it visible to the naked eye at that time.[3] It had a conspicuous red color due to strong Hα line emission.[4] By 1 April 1903 it had faded to magnitude 8.5.[5] By 1989 it had reached visual magnitude 17.38.[6]
DM Geminorum faded from peak brightness by 2 magnitudes in just 6 days, making it a "very fast nova".[7]
All novae are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close together that matter is transferred from the donor to the white dwarf. High speed photometry done with the 1.2 meter telescope at the Whipple Observatory show a small amplitude (0.25 magnitude peak-to-peak) oscillation with a period of 2 hours and 57 minutes, which is probably the orbital period of the binary system. In addition, brightness variations with a period of 22 minutes are also seen in this star's light curve. The star's spectrum and brightness variations are similar to what is seen in intermediate polars.[8]
References
[edit]- 1 2 3 Downes, Ronald; Webbink, Ronald F.; Shara, Michael M. (April 1997). "A Catalog and Atlas of Cataclysmic Variables-Second Edition". Publications of the Astronomical Society of the Pacific. 109: 345. Bibcode:1997PASP..109..345D. doi:10.1086/133900. S2CID 120396435.
- ↑ Shapley, Harlow (January 1933). "The photographic light curves of 11 novae". Annals of the Astronomical Observatory of Harvard College. 84 (5): 121–155. Bibcode:1933AnHar..84..121S. Retrieved 22 January 2021.
- ↑ 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. Retrieved 23 December 2020.
- ↑ Hale, G.E. (May 1903). "The new star in Gemini". The Astrophysical Journal. 17: 300–305. Bibcode:1903ApJ....17..300H. doi:10.1086/141029. Retrieved 23 December 2020.
- ↑ Reese, H.M.; Curtis, H.D. (November 1903). "The spectrum of Nova Geminorum". The Astrophysical Journal. 18: 299–306. Bibcode:1903ApJ....18..299R. doi:10.1086/141071. Retrieved 23 December 2020.
- ↑ Szkody, Paula (August 1994). "BVRGK Observations of Northern Hemisphere Old Novae". The Astronomical Journal. 108: 639. Bibcode:1994AJ....108..639S. doi:10.1086/117098. Retrieved 23 December 2020.
- ↑ Schmidt, Theodor (January 1957). "Die Lichtkurven-Leuchtkraft-Beziehung Neuer Sterne. Mit 8 Textabbildungen". Zeitschrift für Astrophysik. 41: 182. Bibcode:1957ZA.....41..182S.
- ↑ Rodríguez-Gil, P.; Torres, M.A.P. (February 2005). "Time-resolved photometry of the nova remnants". Astronomy and Astrophysics. 431: 289–296. arXiv:astro-ph/0410348. Bibcode:2005A&A...431..289R. doi:10.1051/0004-6361:20041112.
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