V603 Aquilae: Difference between revisions
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'''V603 Aquilae''' (or '''Nova Aquilae 1918''') was a bright [[nova]] occurring in the constellation [[Aquila (constellation)|Aquila]] in 1918. It is a binary system, comprising a white dwarf and donor low-mass star in close orbit to the point of being only semidetached. The white dwarf sucks matter off its companion, which has filled its [[Roche lobe]],<ref name=salvelli>{{cite journal|bibcode=1981ASSL...89..515S|author=Selvelli, P. L.|author2=Cassatella, A. |title=Nova AQL 1918 - A nude old nova |journal=In: Effects of mass loss on stellar evolution; Proceedings of the Fifty-ninth Colloquium, Trieste, Italy, September 15–19, 1980. (A82-33926 16-90) Dordrecht, D. Reidel Publishing Co.|volume=89|pages=515–522|date=1981|doi=10.1007/978-94-009-8500-1_74|series=Astrophysics and Space Science Library|isbn=978-94-009-8502-5}}</ref> onto its [[accretion disk]] and surface until the excess material is blown off in a thermonuclear event.<ref name="johnson13"/> This material then forms an expanding shell, which eventually thins out and disappears.<ref name=salvelli/> |
'''V603 Aquilae''' (or '''Nova Aquilae 1918''') was a bright [[nova]] occurring in the constellation [[Aquila (constellation)|Aquila]] in 1918. It is a binary system, comprising a white dwarf and donor low-mass star in close orbit to the point of being only semidetached. The white dwarf sucks matter off its companion, which has filled its [[Roche lobe]],<ref name=salvelli>{{cite journal|bibcode=1981ASSL...89..515S|author=Selvelli, P. L.|author2=Cassatella, A. |title=Nova AQL 1918 - A nude old nova |journal=In: Effects of mass loss on stellar evolution; Proceedings of the Fifty-ninth Colloquium, Trieste, Italy, September 15–19, 1980. (A82-33926 16-90) Dordrecht, D. Reidel Publishing Co.|volume=89|pages=515–522|date=1981|doi=10.1007/978-94-009-8500-1_74|series=Astrophysics and Space Science Library|isbn=978-94-009-8502-5}}</ref> onto its [[accretion disk]] and surface until the excess material is blown off in a thermonuclear event.<ref name="johnson13"/> This material then forms an expanding shell, which eventually thins out and disappears.<ref name=salvelli/> |
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Discovered on the night of 8 June 1918 by [[A. Grace Cook|Grace Cook]],<ref>{{cite book|last=Mobberley|first=Martin |title=Cataclysmic Cosmic Events and How to Observe Them|publisher=Springer|date=2009|pages=46|isbn=038779946X|url=https://books.google.com/?id=-WQCJOkVfsUC&pg=PA48&dq=Nova+Aquilae+1918#v=onepage&q=Nova%20Aquilae%201918&f=false}}</ref> Nova Aquilae reached a peak [[apparent magnitude|magnitude]] of −0.5; it was the brightest nova recorded in the era of the telescope.<ref name="johnson13">{{cite journal|author=Johnson, Christopher B.|author2=Schaefer, Bradley E.|author3=Kroll , Peter|author4=Henden, Arne A. |date=2013|title=Nova Aquilae 1918 (V603 Aql) Faded by 0.44 mag/century from 1938-2013|url=http://arxiv.org/pdf/1310.6802v2.pdf| arxiv=1310.6802|bibcode = 2014ApJ...780L..25J |doi = 10.1088/2041-8205/780/2/L25|volume=780|issue=2|journal=The Astrophysical Journal|pages=L25}}</ref> It was brighter than all stars bar [[Sirius]] and [[Canopus]].<ref>{{cite book|last=Moore|first=Patrick|title=The Amateur Astronomer|publisher=Springer|date=2006|pages=145|isbn=1846282861|url=https://books.google.com/?id=85RZ04fHe88C&pg=PA145&dq=Nova+Aquilae+1918#v=onepage&q=Nova%20Aquilae%201918&f=false}}</ref> [[SN 1572|Tycho's]] and [[Kepler's Supernova|Kepler's]] supernovae were brighter, but both occurred before the invention of the telescope.<ref>{{cite journal|author=Drechsel, H.|author2=Holm, A.|author3=Krautter, J.|author4=Rahe, J.|last-author-amp=yes|date=1981|title=Phase-dependent optical and ultraviolet observations of the old nova V603 Aquilae (1918)|journal=Astronomy & Astrophysics|volume=99|issue=1|pages=166–72|url=http://adsabs.harvard.edu/full/1981A%26A....99..166D |bibcode=1981A&A....99..166D}}</ref> Originally a star system with a magnitude of 11.43, it took twelve days to fade three magnitudes and then 18.6 years to fade to quiescence.<ref name="johnson13"/> In 1964 [[Robert Kraft (astronomer)|Robert P. Kraft]] ascertained that it was a binary system, recently{{When|date=October 2015}} determined to be true for several other novae at the time.<ref name="kraft64">{{cite journal|last=Kraft|first=Robert P.|date=1964|title=Binary stars among cataclysmic variables. III. Ten old novae|journal=Astrophysical Journal|volume=139|pages= 457–75|url=http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1964ApJ...139..457K&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf|doi=10.1086/147776|bibcode = 1964ApJ...139..457K }}</ref> |
Seen for the first time on the night of 7 June 1918 by [[:pl:Zygmunt Laskowski|Zygmunt Laskowski]], a Polish amateur astronomer, who issued a commemorative medal celebrating his own discovery.<ref>{{Cite web|title=Nova Aquilae 1918|accessdate=24 April 2016|url=http://astrocoins.mrcollector.eu/index.php/english-menu-1/deep-sky/nova-supernova/362-nova-aquilae-1918}}</ref> His discovery might have been unknown or neglected to official authorities. Discovered on the night of 8 June 1918 by [[A. Grace Cook|Grace Cook]],<ref>{{cite book|last=Mobberley|first=Martin |title=Cataclysmic Cosmic Events and How to Observe Them|publisher=Springer|date=2009|pages=46|isbn=038779946X|url=https://books.google.com/?id=-WQCJOkVfsUC&pg=PA48&dq=Nova+Aquilae+1918#v=onepage&q=Nova%20Aquilae%201918&f=false}}</ref> Nova Aquilae reached a peak [[apparent magnitude|magnitude]] of −0.5; it was the brightest nova recorded in the era of the telescope.<ref name="johnson13">{{cite journal|author=Johnson, Christopher B.|author2=Schaefer, Bradley E.|author3=Kroll , Peter|author4=Henden, Arne A. |date=2013|title=Nova Aquilae 1918 (V603 Aql) Faded by 0.44 mag/century from 1938-2013|url=http://arxiv.org/pdf/1310.6802v2.pdf| arxiv=1310.6802|bibcode = 2014ApJ...780L..25J |doi = 10.1088/2041-8205/780/2/L25|volume=780|issue=2|journal=The Astrophysical Journal|pages=L25}}</ref> It was brighter than all stars bar [[Sirius]] and [[Canopus]].<ref>{{cite book|last=Moore|first=Patrick|title=The Amateur Astronomer|publisher=Springer|date=2006|pages=145|isbn=1846282861|url=https://books.google.com/?id=85RZ04fHe88C&pg=PA145&dq=Nova+Aquilae+1918#v=onepage&q=Nova%20Aquilae%201918&f=false}}</ref> [[SN 1572|Tycho's]] and [[Kepler's Supernova|Kepler's]] supernovae were brighter, but both occurred before the invention of the telescope.<ref>{{cite journal|author=Drechsel, H.|author2=Holm, A.|author3=Krautter, J.|author4=Rahe, J.|last-author-amp=yes|date=1981|title=Phase-dependent optical and ultraviolet observations of the old nova V603 Aquilae (1918)|journal=Astronomy & Astrophysics|volume=99|issue=1|pages=166–72|url=http://adsabs.harvard.edu/full/1981A%26A....99..166D |bibcode=1981A&A....99..166D}}</ref> Originally a star system with a magnitude of 11.43, it took twelve days to fade three magnitudes and then 18.6 years to fade to quiescence.<ref name="johnson13"/> In 1964 [[Robert Kraft (astronomer)|Robert P. Kraft]] ascertained that it was a binary system, recently{{When|date=October 2015}} determined to be true for several other novae at the time.<ref name="kraft64">{{cite journal|last=Kraft|first=Robert P.|date=1964|title=Binary stars among cataclysmic variables. III. Ten old novae|journal=Astrophysical Journal|volume=139|pages= 457–75|url=http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1964ApJ...139..457K&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf|doi=10.1086/147776|bibcode = 1964ApJ...139..457K }}</ref> |
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The star system has settled to an average apparent magnitude of 11.4 since the 1940s, fading by around 1/100 of a magnitude per decade. Spectroscopic analysis conducted by Arenas and colleagues indicated the system consisted of a [[white dwarf]] of about 1.2 times as massive as the sun, with an accretion disk, and a companion star with about 20% of the Sun's mass.<ref name=arenas/> This second star is most likely a [[red dwarf]].<ref name=salvelli/> The two stars orbit each other approximately every 3 hours 20 minutes.<ref name=arenas>{{cite journal|bibcode=2000MNRAS.311..135A |title=A spectroscopic study of V603 Aquilae: stellar parameters and continuum-line variations |author=Arenas, J. |author2=Catalán, M. S. |author3=Augusteijn, T. |author4=Retter, A.| journal = [[Monthly Notices of the Royal Astronomical Society]]| volume = 311|issue = 1|pages= 135–48 |url=http://articles.adsabs.harvard.edu/full/2000MNRAS.311..135A |doi=10.1046/j.1365-8711.2000.03061.x|year=2000 }}</ref> |
The star system has settled to an average apparent magnitude of 11.4 since the 1940s, fading by around 1/100 of a magnitude per decade. Spectroscopic analysis conducted by Arenas and colleagues indicated the system consisted of a [[white dwarf]] of about 1.2 times as massive as the sun, with an accretion disk, and a companion star with about 20% of the Sun's mass.<ref name=arenas/> This second star is most likely a [[red dwarf]].<ref name=salvelli/> The two stars orbit each other approximately every 3 hours 20 minutes.<ref name=arenas>{{cite journal|bibcode=2000MNRAS.311..135A |title=A spectroscopic study of V603 Aquilae: stellar parameters and continuum-line variations |author=Arenas, J. |author2=Catalán, M. S. |author3=Augusteijn, T. |author4=Retter, A.| journal = [[Monthly Notices of the Royal Astronomical Society]]| volume = 311|issue = 1|pages= 135–48 |url=http://articles.adsabs.harvard.edu/full/2000MNRAS.311..135A |doi=10.1046/j.1365-8711.2000.03061.x|year=2000 }}</ref> |
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Revision as of 14:53, 24 April 2016
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Right ascension | 18h 48m 54.6366s |
| Declination | +00° 35′ 02.863″ |
| Apparent magnitude (V) | 11.64 |
| Characteristics | |
| Spectral type | sd:Be+ |
| B−V color index | -0.2 ± 0.5 |
| Variable type | Variable star |
| Astrometry | |
| Radial velocity (Rv) | -23 km/s |
| Proper motion (μ) | RA: 10.81 mas/yr Dec.: -8.86 mas/yr |
| Parallax (π) | 4.21 ± 2.59 mas |
| Distance | approx. 800 ly (approx. 200 pc) |
| Absolute magnitude (MV) | 11.65 |
| Details | |
| Radius | 0,72 R☉ |
| Luminosity | -0,14594 L☉ |
| Temperature | 145 K |
| Other designations | |
Nova Aql 1918, Nova Aquilae 1918, EM* CDS 1028, HD 174107, 1RXS J184854.7+003501, ALS 9992, 1ES 1846+00.5, SBC7 706, AN 7.1918, FASTT 1189, HIP 92316, UBV M 51004, CSI+00-18463, GCRV 68659, KPD 1846+0031, 2E 1846.3+0031, LS IV +00 3, 2E 4138, GSC 00448-00423, 2MASS J18485464+0035030, EM* RJHA 116, HBHA 202-05, PLX 4341, AAVSO 1843+00. | |
| Database references | |
| SIMBAD | data |
| Data sources: | |
| Hipparcos Catalogue, CCDM (2002), Bright Star Catalogue (5th rev. ed.) | |
V603 Aquilae (or Nova Aquilae 1918) was a bright nova occurring in the constellation Aquila in 1918. It is a binary system, comprising a white dwarf and donor low-mass star in close orbit to the point of being only semidetached. The white dwarf sucks matter off its companion, which has filled its Roche lobe,[1] onto its accretion disk and surface until the excess material is blown off in a thermonuclear event.[2] This material then forms an expanding shell, which eventually thins out and disappears.[1]
Seen for the first time on the night of 7 June 1918 by Zygmunt Laskowski, a Polish amateur astronomer, who issued a commemorative medal celebrating his own discovery.[3] His discovery might have been unknown or neglected to official authorities. Discovered on the night of 8 June 1918 by Grace Cook,[4] Nova Aquilae reached a peak magnitude of −0.5; it was the brightest nova recorded in the era of the telescope.[2] It was brighter than all stars bar Sirius and Canopus.[5] Tycho's and Kepler's supernovae were brighter, but both occurred before the invention of the telescope.[6] Originally a star system with a magnitude of 11.43, it took twelve days to fade three magnitudes and then 18.6 years to fade to quiescence.[2] In 1964 Robert P. Kraft ascertained that it was a binary system, recently[when?] determined to be true for several other novae at the time.[7]
The star system has settled to an average apparent magnitude of 11.4 since the 1940s, fading by around 1/100 of a magnitude per decade. Spectroscopic analysis conducted by Arenas and colleagues indicated the system consisted of a white dwarf of about 1.2 times as massive as the sun, with an accretion disk, and a companion star with about 20% of the Sun's mass.[8] This second star is most likely a red dwarf.[1] The two stars orbit each other approximately every 3 hours 20 minutes.[8]
References
- ^ a b c Selvelli, P. L.; Cassatella, A. (1981). "Nova AQL 1918 - A nude old nova". In: Effects of mass loss on stellar evolution; Proceedings of the Fifty-ninth Colloquium, Trieste, Italy, September 15–19, 1980. (A82-33926 16-90) Dordrecht, D. Reidel Publishing Co. Astrophysics and Space Science Library. 89: 515–522. Bibcode:1981ASSL...89..515S. doi:10.1007/978-94-009-8500-1_74. ISBN 978-94-009-8502-5.
- ^ a b c Johnson, Christopher B.; Schaefer, Bradley E.; Kroll , Peter; Henden, Arne A. (2013). "Nova Aquilae 1918 (V603 Aql) Faded by 0.44 mag/century from 1938-2013" (PDF). The Astrophysical Journal. 780 (2): L25. arXiv:1310.6802. Bibcode:2014ApJ...780L..25J. doi:10.1088/2041-8205/780/2/L25.
- ^ "Nova Aquilae 1918". Retrieved 24 April 2016.
- ^ Mobberley, Martin (2009). Cataclysmic Cosmic Events and How to Observe Them. Springer. p. 46. ISBN 038779946X.
- ^ Moore, Patrick (2006). The Amateur Astronomer. Springer. p. 145. ISBN 1846282861.
- ^ Drechsel, H.; Holm, A.; Krautter, J.; Rahe, J. (1981). "Phase-dependent optical and ultraviolet observations of the old nova V603 Aquilae (1918)". Astronomy & Astrophysics. 99 (1): 166–72. Bibcode:1981A&A....99..166D.
{{cite journal}}: Unknown parameter|last-author-amp=ignored (|name-list-style=suggested) (help) - ^ Kraft, Robert P. (1964). "Binary stars among cataclysmic variables. III. Ten old novae" (PDF). Astrophysical Journal. 139: 457–75. Bibcode:1964ApJ...139..457K. doi:10.1086/147776.
- ^ a b Arenas, J.; Catalán, M. S.; Augusteijn, T.; Retter, A. (2000). "A spectroscopic study of V603 Aquilae: stellar parameters and continuum-line variations". Monthly Notices of the Royal Astronomical Society. 311 (1): 135–48. Bibcode:2000MNRAS.311..135A. doi:10.1046/j.1365-8711.2000.03061.x.
- Pottasch, Stuart (1959). "The nova outburst: V. The temperature and radius of the central exciting star and observation" (PDF). SAO/NASA Astrophysics Data System (ADS). 22: 416. Bibcode:1959AnAp...22..412P.
- Image V603 Aquilae
