DI Lacertae on:
[Wikipedia]
[Google]
[Amazon]
DI Lacertae or Nova Lacertae 1910 was a nova in constellation Lacerta (constellation), Lacerta which appeared in 1910. It was discovered by T. H. E. C. Espin, Thomas Henry Espinell Compton Espin at Wolsingham Observatory on 30 Dec 1910, at which time it was an 8th apparent magnitude, magnitude object. Subsequent examination of pre-discovery Photographic_plate#Astronomy, photographic plates showed that the outburst occurred sometime between 17 November 1910 and 23 November 1910. It reached a peak brightness of magnitude 4.6 on 26 November 1910, making it visible to the naked eye. Before the nova event DI Lacertae was a 14th magnitude star, and by 1950 it had returned to 14th magnitude.
DI Lacertae dropped from peak brightness by 3 magnitudes in just 43 days, making it a "fast nova".
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. The mass of the white dwarf has been estimated to be 0.91±0.2
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 10−10 per year with a 30,000 Kelvin white dwarf. Darnley ''et al.'' argue that the donor star is probably a main sequence star or, less probably, a subdwarf.
DI Lacertae or Nova Lacertae 1910 was a nova in constellation Lacerta (constellation), Lacerta which appeared in 1910. It was discovered by T. H. E. C. Espin, Thomas Henry Espinell Compton Espin at Wolsingham Observatory on 30 Dec 1910, at which time it was an 8th apparent magnitude, magnitude object. Subsequent examination of pre-discovery Photographic_plate#Astronomy, photographic plates showed that the outburst occurred sometime between 17 November 1910 and 23 November 1910. It reached a peak brightness of magnitude 4.6 on 26 November 1910, making it visible to the naked eye. Before the nova event DI Lacertae was a 14th magnitude star, and by 1950 it had returned to 14th magnitude.
DI Lacertae dropped from peak brightness by 3 magnitudes in just 43 days, making it a "fast nova".
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. The mass of the white dwarf has been estimated to be 0.91±0.2
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 10−10 per year with a 30,000 Kelvin white dwarf. Darnley ''et al.'' argue that the donor star is probably a main sequence star or, less probably, a subdwarf.
References
Novae Lacerta 1910 in science Objects with variable star designations, Lacertae, DI Henry Draper Catalogue objects, 214239 {{var-star-stub