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CK Vulpeculae

April 10, 2024

CK Vulpeculae (also Nova Vulpeculae 1670) is an object whose exact nature is unknown.[4] It was once considered to be the oldest reliably-documented nova. It consists of a compact central object surrounded by a bipolar nebula.

CK Vulpeculae

CK Vulpeculae taken by ALMA.[1]
Credit: ALMA (ESO/NAOJ/NRAO)/S. P. S. Eyres
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Vulpecula
Right ascension 19h 47m 38.0s[2]
Declination +27° 18′ 48″[2]
Apparent magnitude (V) max 2.6[2]
Characteristics
B−V color index 0.7[3]
Variable type unknown[3]
Astrometry
Distance10000+3000
−2000[4] ly
(3200+900
−600[4] pc)
Details
Luminosity0.9[3] L☉
Temperature14,000 – 100,000[3] K
Other designations
CK Vulpeculae, CK Vul, Nova Vul 1670, HR 7539, 11 Vul[5]
Database references
SIMBADdata

Models suggest CK Vulpeculae may not be a classic nova; rather it may be classified as a luminous red nova which is the result of two main sequence stars colliding and merging. A 2018 study found it was most likely the result of an unusual collision of a white dwarf and a brown dwarf. A 2020 article ruled out this proposed mechanism and proposes that CK Vulpeculae is an intermediate luminosity optical transient, i.e. an object in the luminosity gap between supernovae and novae.[4]

Eruptive history edit

 
Position of the 1670 Nova near Albireo
 
The location of CK Vulpeculae (circled in red)

CK Vulpeculae was discovered on June 20, 1670, by Voituret Anthelme and independently on July 25 by Johannes Hevelius. It had a brightness maximum of approximately magnitude 3 at its discovery after which it faded. A second maximum of approximately 2.6 magnitude was observed in March 1671, after which Johannes Hevelius and Giovanni Cassini observed it throughout spring and summer until it faded from naked-eye view in late August 1671. A last weakly visible brightness maximum of approximately 5.5 to 6 magnitude was observed by Hevelius in March 1672 and finally faded from view late May.[6]

This was the first nova for which there are multiple and reliable observations. The next nova to be documented as comprehensively was Nova Ophiuchi 1841.[6]

Identification edit

 
Visible light is in blue, submillimeter radiation map highlighted in green, and molecular emission in red.

John Flamsteed, who was elaborating his catalogue during these years, assigned the star the Flamsteed designation 11 Vulpeculae,[5] which has been noted later by Francis Baily as one of Flamsteed's lost stars, because it had not been detectable for centuries.[7]

In 1981, a point source near the centre of a small nebula was identified as CK Vulpeculae, with an estimated red magnitude of 20.7.[8][6] Later observations cast doubt on that identification,[9] and it is now known to be a background object. That object and another star are thought to be seen though dense nebulosity associated with CK Vulpeculae which causes them to vary dramatically in brightness.[10]

CK Vulpeculae now consists of a compact central object with gas flowing out at approximately 210 km/s into a bipolar nebula.[10] A 15" path of nebulosity seen in the 1980s lies at the centre of a 70" bipolar nebula.[11] A compact radio source is seen at the centre of this nebula, and an infrared point source, but it has not been detected at optical wavelengths.[3] The ionisation of the nebula and its radio emission indicate that the central source is still very hot and relatively luminous.[12][10] It is either inside of a cloud of cold (~ 15 K) dust or the cloud is in front of it from the Earth's perspective. Molecular gas in the vicinity is rich in nitrogen relative to oxygen.[12]

Properties edit

 
Radioactive molecules in the remains of a stellar collision.[13]

The luminosity of the central object, estimated from infrared dust emission, is about 0.9 L☉.[3] The luminosity required to energise the observed nebulosity is calculated at 3 L☉ from an object at 60,000 K[10] At the time of its eruption, the luminosity of CK Vulpeculae is calculated to have been at least 7,000,000 L☉.[4] Known ionic emission lines in the spectrum, and unidentified absorption features in the infrared indicate a temperature between 14,000 K and 100,000 K.[3]

Astronomers using the Atacama Large Millimetre Array (ALMA) and the Northern Extended Millimeter Array (NOEMA) radio telescopes to study CK Vulpeculae have found the first convincing evidence of a radioactive molecule outside the Earth's Solar System, which is aluminium monofluoride as the 26Al isotopologue.[14]

Nature of the eruption edit

In the past, a luminous red nova merger, very late thermal pulse, or a diffusion-induced nova have all been suggested but there are problems with all these explanations.[3] An analysis of the structures and isotopic abundances in the remaining nebula using the Atacama Large Millimeter Array (ALMA) in 2018 concluded that the nova and associated nebula were caused by the unusual merger of a white dwarf and brown dwarf between 1670 and 1672.[15] Although it was previously considered to be located about 2,280 ly (700 pc) away,[10] a 2020 paper ruled this out due to a larger distance for CK Vulpeculae making the intrinsic energy release too great for a stellar merger. Instead the 2020 paper concludes that the CK Vulpeculae outburst was an intermediate luminosity optical transient with an unknown cause.[4]

References edit

  1. ^ "Through the Hourglass". www.eso.org. Retrieved 8 October 2018.
  2. ^ a b c Downes, Ronald A; Webbink, Ronald F; Shara, Michael M; Ritter, Hans; Kolb, Ulrich; Duerbeck, Hilmar W (2001). "A Catalog and Atlas of Cataclysmic Variables: The Living Edition". The Publications of the Astronomical Society of the Pacific. 113 (784): 764. arXiv:astro-ph/0102302. Bibcode:2001PASP..113..764D. doi:10.1086/320802. S2CID 16285959.
  3. ^ a b c d e f g h Evans, A.; et al. (2016). "CK Vul: A smorgasbord of hydrocarbons rules out a 1670 nova (and much else besides)". Monthly Notices of the Royal Astronomical Society. 457 (3): 2871–2876. arXiv:1512.02146. Bibcode:2016MNRAS.457.2871E. doi:10.1093/mnras/stw352. S2CID 76657165.
  4. ^ a b c d e f Banerjee, D. P. K.; Geballe, T. R.; Evans, A.; Shahbandeh, M.; Woodward, C. E.; Gehrz, R. D.; Eyres, S. P. S.; Starrfield, S.; Zijlstra, A. (2020). "Near-infrared Spectroscopy of CK Vulpeculae: Revealing a Remarkably Powerful Blast from the Past". The Astrophysical Journal. 904 (2): L23. arXiv:2011.02939. Bibcode:2020ApJ...904L..23B. doi:10.3847/2041-8213/abc885. S2CID 226254757.
  5. ^ a b Morton, Wagman (2003). Lost Stars. Blacksburg, Virginia: McDonald and Woodward. p. 494. ISBN 978-0-939923-78-6.
  6. ^ a b c Shara, M. M.; Moffat, A. F. J.; Webbink, R. F. (July 1, 1985). "Unraveling the oldest and faintest recovered nova - CK Vulpeculae (1670)". Astrophysical Journal. 294: 271–285. Bibcode:1985ApJ...294..271S. doi:10.1086/163296.
  7. ^ Baily, Francis (1845). The Catalogue of Stars of the British Association for the Advancement of Science. London: Richard and John E Taylor. p. 77. Bibcode:1845tcot.book.....B. ISBN 978-1165133253.
  8. ^ Shara, M. M.; Moffat, A. F. J. (July 1, 1982). "The recovery of CK Vulpeculae (Nova 1670) - The oldest 'old nova'". Astronomical Journal. 258 (Part 2 Letters to the Editor): L41–L44. Bibcode:1982ApJ...258L..41S. doi:10.1086/183826.
  9. ^ Naylor, T.; Charles, P. A.; Mukai, K.; Evans, A. (1992). "An observational case against nova hibernation". Monthly Notices of the Royal Astronomical Society. 258 (3): 449–456. Bibcode:1992MNRAS.258..449N. doi:10.1093/mnras/258.3.449.
  10. ^ a b c d e Hajduk, M.; van Hoof, P. A. M.; Zijlstra, A. A. (11 June 2013). "CK Vul: evolving nebula and three curious background stars". Monthly Notices of the Royal Astronomical Society. 432 (1): 167–175. arXiv:1312.5846. Bibcode:2013MNRAS.432..167H. doi:10.1093/mnras/stt426. S2CID 118475362.
  11. ^ Hajduk, M; Zijlstra, Albert A; Van Hoof, P. A. M; Lopez, J. A; Drew, J. E; Evans, A; Eyres, S. P. S; Gesicki, K; Greimel, R; Kerber, F; Kimeswenger, S; Richer, M. G (2007). "The enigma of the oldest 'nova': The central star and nebula of CK Vul". Monthly Notices of the Royal Astronomical Society. 378 (4): 1298–1308. arXiv:0709.3746. Bibcode:2007MNRAS.378.1298H. doi:10.1111/j.1365-2966.2007.11825.x. S2CID 14892116.
  12. ^ a b Kaminski, Tomasz; Menten, Karl M.; Tylenda, Romuald; Hajduk, Marcin; Patel, Nimesh A.; Kraus, Alexander (March 23, 2015). "Nuclear ashes and outflow in the eruptive star Nova Vul 1670". Nature. 520 (7547): 322–4. arXiv:1503.06570. Bibcode:2015Natur.520..322K. doi:10.1038/nature14257. PMID 25799986. S2CID 4449518.
  13. ^ "Stellar Corpse Reveals Origin of Radioactive Molecules - Observations using ALMA find radioactive isotope aluminium-26 from the remnant CK Vulpeculae". www.eso.org. Retrieved 31 July 2018.
  14. ^ Kamiński, T; Menten, K. M; Tylenda, R; Karakas, A; Belloche, A; Patel, N. A (2017). "Organic molecules, ions, and rare isotopologues in the remnant of the stellar-merger candidate, CK Vulpeculae (Nova 1670)". Astronomy & Astrophysics. 607: A78. arXiv:1708.02261. Bibcode:2017A&A...607A..78K. doi:10.1051/0004-6361/201731287. S2CID 62829732.
  15. ^ Eyres, Stewart; Evans, Aneurin; Zijlstra, Albert; Avison, Adam; Gehrz, Robert; Hajduk, Marcin; Starrfield, Sumner; Mohamed, Shazrene; Woodward, Charles; Wagner, R. Mark (16 September 2018). "ALMA reveals the aftermath of a white dwarf--brown dwarf merger in CK Vulpeculae". Monthly Notices of the Royal Astronomical Society. 481 (4): 4931. arXiv:1809.05849. Bibcode:2018MNRAS.481.4931E. doi:10.1093/mnras/sty2554. S2CID 119462149.

External links edit

April 10, 2024
vulpeculae, also, nova, vulpeculae, 1670, object, whose, exact, nature, unknown, once, considered, oldest, reliably, documented, nova, consists, compact, central, object, surrounded, bipolar, nebula, taken, alma, credit, alma, naoj, nrao, eyresobservation, dat. CK Vulpeculae also Nova Vulpeculae 1670 is an object whose exact nature is unknown 4 It was once considered to be the oldest reliably documented nova It consists of a compact central object surrounded by a bipolar nebula CK VulpeculaeCK Vulpeculae taken by ALMA 1 Credit ALMA ESO NAOJ NRAO S P S EyresObservation dataEpoch J2000 0 Equinox J2000 0Constellation VulpeculaRight ascension 19h 47m 38 0s 2 Declination 27 18 48 2 Apparent magnitude V max 2 6 2 CharacteristicsB V color index 0 7 3 Variable type unknown 3 AstrometryDistance10000 3000 2000 4 ly 3200 900 600 4 pc DetailsLuminosity0 9 3 L Temperature14 000 100 000 3 KOther designationsCK Vulpeculae CK Vul Nova Vul 1670 HR 7539 11 Vul 5 Database referencesSIMBADdataModels suggest CK Vulpeculae may not be a classic nova rather it may be classified as a luminous red nova which is the result of two main sequence stars colliding and merging A 2018 study found it was most likely the result of an unusual collision of a white dwarf and a brown dwarf A 2020 article ruled out this proposed mechanism and proposes that CK Vulpeculae is an intermediate luminosity optical transient i e an object in the luminosity gap between supernovae and novae 4 Contents 1 Eruptive history 2 Identification 3 Properties 4 Nature of the eruption 5 References 6 External linksEruptive history edit nbsp Position of the 1670 Nova near Albireo nbsp The location of CK Vulpeculae circled in red CK Vulpeculae was discovered on June 20 1670 by Voituret Anthelme and independently on July 25 by Johannes Hevelius It had a brightness maximum of approximately magnitude 3 at its discovery after which it faded A second maximum of approximately 2 6 magnitude was observed in March 1671 after which Johannes Hevelius and Giovanni Cassini observed it throughout spring and summer until it faded from naked eye view in late August 1671 A last weakly visible brightness maximum of approximately 5 5 to 6 magnitude was observed by Hevelius in March 1672 and finally faded from view late May 6 This was the first nova for which there are multiple and reliable observations The next nova to be documented as comprehensively was Nova Ophiuchi 1841 6 Identification edit nbsp Visible light is in blue submillimeter radiation map highlighted in green and molecular emission in red John Flamsteed who was elaborating his catalogue during these years assigned the star the Flamsteed designation 11 Vulpeculae 5 which has been noted later by Francis Baily as one of Flamsteed s lost stars because it had not been detectable for centuries 7 In 1981 a point source near the centre of a small nebula was identified as CK Vulpeculae with an estimated red magnitude of 20 7 8 6 Later observations cast doubt on that identification 9 and it is now known to be a background object That object and another star are thought to be seen though dense nebulosity associated with CK Vulpeculae which causes them to vary dramatically in brightness 10 CK Vulpeculae now consists of a compact central object with gas flowing out at approximately 210 km s into a bipolar nebula 10 A 15 path of nebulosity seen in the 1980s lies at the centre of a 70 bipolar nebula 11 A compact radio source is seen at the centre of this nebula and an infrared point source but it has not been detected at optical wavelengths 3 The ionisation of the nebula and its radio emission indicate that the central source is still very hot and relatively luminous 12 10 It is either inside of a cloud of cold 15 K dust or the cloud is in front of it from the Earth s perspective Molecular gas in the vicinity is rich in nitrogen relative to oxygen 12 Properties edit nbsp Radioactive molecules in the remains of a stellar collision 13 The luminosity of the central object estimated from infrared dust emission is about 0 9 L 3 The luminosity required to energise the observed nebulosity is calculated at 3 L from an object at 60 000 K 10 At the time of its eruption the luminosity of CK Vulpeculae is calculated to have been at least 7 000 000 L 4 Known ionic emission lines in the spectrum and unidentified absorption features in the infrared indicate a temperature between 14 000 K and 100 000 K 3 Astronomers using the Atacama Large Millimetre Array ALMA and the Northern Extended Millimeter Array NOEMA radio telescopes to study CK Vulpeculae have found the first convincing evidence of a radioactive molecule outside the Earth s Solar System which is aluminium monofluoride as the 26Al isotopologue 14 Nature of the eruption editIn the past a luminous red nova merger very late thermal pulse or a diffusion induced nova have all been suggested but there are problems with all these explanations 3 An analysis of the structures and isotopic abundances in the remaining nebula using the Atacama Large Millimeter Array ALMA in 2018 concluded that the nova and associated nebula were caused by the unusual merger of a white dwarf and brown dwarf between 1670 and 1672 15 Although it was previously considered to be located about 2 280 ly 700 pc away 10 a 2020 paper ruled this out due to a larger distance for CK Vulpeculae making the intrinsic energy release too great for a stellar merger Instead the 2020 paper concludes that the CK Vulpeculae outburst was an intermediate luminosity optical transient with an unknown cause 4 References edit Through the Hourglass www eso org Retrieved 8 October 2018 a b c Downes Ronald A Webbink Ronald F Shara Michael M Ritter Hans Kolb Ulrich Duerbeck Hilmar W 2001 A Catalog and Atlas of Cataclysmic Variables The Living Edition The Publications of the Astronomical Society of the Pacific 113 784 764 arXiv astro ph 0102302 Bibcode 2001PASP 113 764D doi 10 1086 320802 S2CID 16285959 a b c d e f g h Evans A et al 2016 CK Vul A smorgasbord of hydrocarbons rules out a 1670 nova and much else besides Monthly Notices of the Royal Astronomical Society 457 3 2871 2876 arXiv 1512 02146 Bibcode 2016MNRAS 457 2871E doi 10 1093 mnras stw352 S2CID 76657165 a b c d e f Banerjee D P K Geballe T R Evans A Shahbandeh M Woodward C E Gehrz R D Eyres S P S Starrfield S Zijlstra A 2020 Near infrared Spectroscopy of CK Vulpeculae Revealing a Remarkably Powerful Blast from the Past The Astrophysical Journal 904 2 L23 arXiv 2011 02939 Bibcode 2020ApJ 904L 23B doi 10 3847 2041 8213 abc885 S2CID 226254757 a b Morton Wagman 2003 Lost Stars Blacksburg Virginia McDonald and Woodward p 494 ISBN 978 0 939923 78 6 a b c Shara M M Moffat A F J Webbink R F July 1 1985 Unraveling the oldest and faintest recovered nova CK Vulpeculae 1670 Astrophysical Journal 294 271 285 Bibcode 1985ApJ 294 271S doi 10 1086 163296 Baily Francis 1845 The Catalogue of Stars of the British Association for the Advancement of Science London Richard and John E Taylor p 77 Bibcode 1845tcot book B ISBN 978 1165133253 Shara M M Moffat A F J July 1 1982 The recovery of CK Vulpeculae Nova 1670 The oldest old nova Astronomical Journal 258 Part 2 Letters to the Editor L41 L44 Bibcode 1982ApJ 258L 41S doi 10 1086 183826 Naylor T Charles P A Mukai K Evans A 1992 An observational case against nova hibernation Monthly Notices of the Royal Astronomical Society 258 3 449 456 Bibcode 1992MNRAS 258 449N doi 10 1093 mnras 258 3 449 a b c d e Hajduk M van Hoof P A M Zijlstra A A 11 June 2013 CK Vul evolving nebula and three curious background stars Monthly Notices of the Royal Astronomical Society 432 1 167 175 arXiv 1312 5846 Bibcode 2013MNRAS 432 167H doi 10 1093 mnras stt426 S2CID 118475362 Hajduk M Zijlstra Albert A Van Hoof P A M Lopez J A Drew J E Evans A Eyres S P S Gesicki K Greimel R Kerber F Kimeswenger S Richer M G 2007 The enigma of the oldest nova The central star and nebula of CK Vul Monthly Notices of the Royal Astronomical Society 378 4 1298 1308 arXiv 0709 3746 Bibcode 2007MNRAS 378 1298H doi 10 1111 j 1365 2966 2007 11825 x S2CID 14892116 a b Kaminski Tomasz Menten Karl M Tylenda Romuald Hajduk Marcin Patel Nimesh A Kraus Alexander March 23 2015 Nuclear ashes and outflow in the eruptive star Nova Vul 1670 Nature 520 7547 322 4 arXiv 1503 06570 Bibcode 2015Natur 520 322K doi 10 1038 nature14257 PMID 25799986 S2CID 4449518 Stellar Corpse Reveals Origin of Radioactive Molecules Observations using ALMA find radioactive isotope aluminium 26 from the remnant CK Vulpeculae www eso org Retrieved 31 July 2018 Kaminski T Menten K M Tylenda R Karakas A Belloche A Patel N A 2017 Organic molecules ions and rare isotopologues in the remnant of the stellar merger candidate CK Vulpeculae Nova 1670 Astronomy amp Astrophysics 607 A78 arXiv 1708 02261 Bibcode 2017A amp A 607A 78K doi 10 1051 0004 6361 201731287 S2CID 62829732 Eyres Stewart Evans Aneurin Zijlstra Albert Avison Adam Gehrz Robert Hajduk Marcin Starrfield Sumner Mohamed Shazrene Woodward Charles Wagner R Mark 16 September 2018 ALMA reveals the aftermath of a white dwarf brown dwarf merger in CK Vulpeculae Monthly Notices of the Royal Astronomical Society 481 4 4931 arXiv 1809 05849 Bibcode 2018MNRAS 481 4931E doi 10 1093 mnras sty2554 S2CID 119462149 External links edithttp www space com 28907 oldest nova astronomy mystery html http www sci news com astronomy science ground based telescopes nova ck vulpeculae 02626 html https www astronews ru cgi bin mng cgi page news amp news 11336 Retrieved from https en wikipedia org w index php title CK Vulpeculae amp oldid 1174811417, wikipedia, wiki, book, books, library,

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