DI Lacertae

{{Starbox begin

| name=DI Lacertae}}

{{Starbox image

| image=

{{Location mark

|image=DILacLocation.png|alt=|width=280

}}

|caption=Location of DI Lacertae (circled in red)

}}

{{Starbox observe

| epoch=J2000.0 (ICRS)

| ra={{RA|22|35|48.495}}

| dec={{DEC|52|42|59.64}}

| appmag_v=4.6v{{snd}}14.9p

| constell=Lacerta

}}

{{Starbox character

| class =

| variable = Nova

}}

{{Starbox astrometry

| radial_v =

| prop_mo_ra = −1.794

| prop_mo_dec = −2.362

| parallax = 0.5783

| p_error = 0.0173

| parallax_footnote =

| absmag_v = −7.2{{snd}}+3.8

}}

{{Starbox detail

| component1 = White dwarf

| mass = 0.91

}}

{{Starbox catalog

| names=Nova Lac 1910, DI Lac, HD 214239, AAVSO 2231+52

}}

{{Starbox reference

| Simbad=V*+DI+Lac

}}

File:DILacLightCurve.png of nova DI Lacertae, plotted from data presented by Shapley. If multiple measurements with identical times were reported, they were averaged before plotting The red pre-eruption point is from Robinson.]]

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. 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 orbital 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{{solar mass|link=y}}

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{{solar mass}} 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

{{reflist|refs=

{{cite journal |last1=Darnley |first1=M.J. |last2=Ribeiro |first2=V.A.R.M. |last3=Bode |first3=M.F. |last4=Hounsell |first4=R.A. |last5=Williams |first5=R.P. |title=On the Progenitors of Galactic Novae |journal=The Astrophysical Journal |date=February 2012 |volume=746 |issue=1 |page=61 |doi=10.1088/0004-637X/746/1/61 |arxiv=1112.2589 |bibcode=2012ApJ...746...61D |s2cid=119291027 }}

{{cite journal |last1=Ritter |first1=H. |last2=Kolb |first2=U. |title=Catalogue of cataclysmic binaries, low-mass X-ray binaries and related objects (Seventh edition) |journal=Astronomy and Astrophysics |date=June 2003 |volume=404 |pages=301–303 |doi=10.1051/0004-6361:20030330 |arxiv=astro-ph/0301444 |bibcode=2003A&A...404..301R |doi-access=free }}

{{cite journal |last1=Marin |first1=E. |last2=Shafter |first2=A.W. |title=The Orbital Period of V368 Aquilae (Nova Aquilae 1936 No. 2 |journal=Publications of the Astronomical Society of the Pacific |date=October 2009 |volume=121 |issue=884 |page=1090 |doi=10.1086/644647 |arxiv=0908.3703 |bibcode=2009PASP..121.1090M |s2cid=119192314 }}

{{cite journal |last1=Steavenson |first1=W.H. |title=Observations of novae, 1950, 1951 and 1952 |journal=Monthly Notices of the Royal Astronomical Society |date=January 1953 |volume=113 |issue=2 |page=258 |doi=10.1093/mnras/113.2.258 |bibcode=1953MNRAS.113..258S |doi-access=free }}

{{cite journal |last1=Selvelli |first1=Pierluigi |last2=Gilmozzi |first2=Roberto |title=A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD |journal=Astronomy & Astrophysics |date=February 2019 |volume=622 |pages=A186 |doi=10.1051/0004-6361/201834238 |arxiv=1903.05868 |bibcode=2019A&A...622A.186S |doi-access=free }}

{{cite journal |last1=Duerbeck |first1=Hilmar W. |title=A Reference Catalogue and Atlas of Galactic Novae |journal=Space Science Reviews |date=March 1987 |volume=45 |issue=1–2 |pages=1–14 |doi=10.1007/BF00187826 |bibcode=1987SSRv...45....1D |s2cid=115854775 }}

{{cite journal |last1=Downes |first1=Ronald |last2=Webbink |first2=Ronald F. |last3=Shara |first3=Michael M. |title=A Catalog and Atlas of Cataclysmic Variables-Second Edition |journal=Publications of the Astronomical Society of the Pacific |date=April 1997 |volume=109 |page=345 |doi=10.1086/133900 |bibcode=1997PASP..109..345D |s2cid=120396435 |doi-access=free }}

{{cite journal | title=Observations of Nova Lacertae at the Yerkes Observatory | last1=Frost | first1=E. B. | journal=The Astrophysical Journal | volume=33 | pages=410–417 | year=1911 | bibcode=1911ApJ....33..410F | doi=10.1086/141865 }}

{{cite journal | title=Far Ultraviolet Spectroscopy of Old Novae. II. RR Pic, V533 Her, and DI Lac | last1=Sion | first1=Edward M. | last2=Godon | first2=Patrick | last3=Jones | first3=Liam | display-authors=1 | journal=The Astronomical Journal | volume=153 | issue=3 | at=109 | year=2017 | arxiv=1701.05218 | bibcode=2017AJ....153..109S | doi=10.3847/1538-3881/153/3/109 | pmid=29456254 | pmc=5810142 | doi-access=free }}

{{cite journal |last1=Shapley |first1=Harlow |title=The photographic light curves of 11 novae |journal=Annals of the Astronomical Observatory of Harvard College |date=January 1933 |volume=84 |issue=5 |pages=121–155 |bibcode=1933AnHar..84..121S }}

{{cite journal |last1=Robinson |first1=E.L. |title=Preeruption light curves of novae |journal=Astronomical Journal |date=July 1975 |volume=80 |pages=515–524 |doi=10.1086/111774 |bibcode=1975AJ.....80..515R }}

}}

Category:Novae

Category:Lacerta

Category:1910 in science

Lacertae, DI

214239