Astronomy:DI Lacertae
 | |
| Observation data Epoch J2000.0 Equinox (celestial coordinates) | |
|---|---|
| Constellation | Lacerta |
| Right ascension | 22h 35m 48.495s[1] |
| Declination | 52° 42′ 59.64″[1] |
| Apparent magnitude (V) | 4.6v – 14.9p[2] |
| Characteristics | |
| Variable type | Nova |
| Astrometry | |
| Proper motion (μ) | RA: −1.794[1] mas/yr Dec.: −2.362[1] mas/yr |
| Parallax (π) | 0.5783 ± 0.0173[1] mas |
| Distance | 5,600 ± 200 ly (1,730 ± 50 pc) |
| Absolute magnitude (MV) | −7.2 – +3.8[3] |
| Details | |
| White dwarf | |
| Mass | 0.91[3] M☉ |
| Other designations | |
Nova Lac 1910, DI Lac, HD 214239, AAVSO 2231+52 | |
| Database references | |
| SIMBAD | data |
DI Lacertae or Nova Lacertae 1910 was a nova in constellation Lacerta which appeared in 1910. It was discovered by Thomas Henry Espinell Compton Espin at Wolsingham Observatory on 30 Dec 1910, at which time it was an 8th magnitude object. Subsequent examination of pre-discovery photographic plates showed that the outburst occurred sometime between 17 November 1910 and 23 November 1910.[6] It reached a peak brightness of magnitude 4.6 on 26 November 1910, making it visible to the naked eye.[3][4] Before the nova event DI Lacertae was a 14th magnitude star,[7] and by 1950 it had returned to 14th magnitude.[8]
DI Lacertae dropped from peak brightness by 3 magnitudes in just 43 days, making it a "fast nova".[9][10]
All novae are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close to each other that matter is transferred from the donor star to the white dwarf. In the case of DI Lacertae, the oribital period for the binary pair is 13.050 hours, which is unusually long for a nova.[11] The mass of the white dwarf has been estimated to be 0.91±0.2M☉ In 2017 Sion et al. presented analysis of ultraviolet spectra from the Far Ultraviolet Spectroscopic Explorer and International Ultraviolet Explorer spacecraft, and found the best fit for DI Lacertae to be an accretion disk with a mass accretion rate of 10−10M☉ per year with a 30,000 Kelvin white dwarf.[12] Darnley et al. argue that the donor star is probably a main sequence star or, less probably, a subdwarf.[11]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 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. doi:10.1086/133900. Bibcode: 1997PASP..109..345D.
- ↑ 3.0 3.1 3.2 Selvelli, Pierluigi; Gilmozzi, Roberto (February 2019). "A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD". Astronomy & Astrophysics 622: A186. doi:10.1051/0004-6361/201834238. Bibcode: 2019A&A...622A.186S.
- ↑ 4.0 4.1 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.
- ↑ Robinson, E.L. (July 1975). "Preeruption light curves of novae". Astronomical Journal 80: 515–524. doi:10.1086/111774. Bibcode: 1975AJ.....80..515R.
- ↑ Duerbeck, Hilmar W. (March 1987). "A Reference Catalogue and Atlas of Galactic Novae". Space Science Reviews 45 (1–2): 1–14. doi:10.1007/BF00187826. Bibcode: 1987SSRv...45....1D.
- ↑ Frost, E. B. (1911). "Observations of Nova Lacertae at the Yerkes Observatory". The Astrophysical Journal 33: 410–417. doi:10.1086/141865. Bibcode: 1911ApJ....33..410F.
- ↑ Steavenson, W.H. (January 1953). "Observations of novae, 1950, 1951 and 1952". Monthly Notices of the Royal Astronomical Society 113 (2): 258. doi:10.1093/mnras/113.2.258. Bibcode: 1953MNRAS.113..258S.
- ↑ Marin, E.; Shafter, A.W. (October 2009). "The Orbital Period of V368 Aquilae (Nova Aquilae 1936 No. 2". Publications of the Astronomical Society of the Pacific 121 (884): 1090. doi:10.1086/644647. Bibcode: 2009PASP..121.1090M.
- ↑ Ritter, H.; Kolb, U. (June 2003). "Catalogue of cataclysmic binaries, low-mass X-ray binaries and related objects (Seventh edition)". Astronomy and Astrophysics 404: 301–303. doi:10.1051/0004-6361:20030330. Bibcode: 2003A&A...404..301R.
- ↑ 11.0 11.1 Darnley, M.J.; Ribeiro, V.A.R.M.; Bode, M.F.; Hounsell, R.A.; Williams, R.P. (February 2012). "On the Progenitors of Galactic Novae". The Astrophysical Journal 746 (1): 61. doi:10.1088/0004-637X/746/1/61. Bibcode: 2012ApJ...746...61D.
- ↑ Sion, Edward M. et al. (2017). "Far Ultraviolet Spectroscopy of Old Novae. II. RR Pic, V533 Her, and DI Lac". The Astronomical Journal 153 (3): 109. doi:10.3847/1538-3881/153/3/109. PMID 29456254. Bibcode: 2017AJ....153..109S.
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