V Puppis

A 2025 study combining all previous eclipse data and [[astrometry]] from the [[Hipparcos]] and [[Gaia (spacecraft)|Gaia]] spacecrafts again suggested the presence of an outer companion. The period, semi-major axis and mass were revised to 14.034 years, 17.88 au and {{solar mass|7.73}}. Additional data could confirm the nature of this object as either a black hole or a B-type main-sequence star that was not direcly detected yet. If the companion were a B-type star, it would explain the third light contribution found by the 2021 publication but not the apparent non-detection in the spectrum.{{cite journal |last1=Xiao |first1=Guang-Yao |last2=Feng |first2=Fabo |last3=Wang |first3=Song |last4=Li |first4=Kai |last5=Rui |first5=Yicheng |last6=Duan |first6=Xiao-Wei |title=Detection of dark companions via the combination of eclipse timing variation, Hipparcos and/Or Gaia astrometry: The cases of V Puppis and CY Ari |date=2025 |journal=The Astrophysical Journal |arxiv=2512.20087}} If V Puppis were confirmed to harbour a black hole, it would be among the [[list of nearest known black holes|closest-known]], with a similar distance to the current leader, [[Gaia BH1]].

A 2025 study combining all previous eclipse data and [[astrometry]] from the [[Hipparcos]] and [[Gaia (spacecraft)|Gaia]] spacecrafts again suggested the presence of an outer companion. The period, semi-major axis and mass were revised to 14.034 years, 17.88 au and {{solar mass|7.73}}. Additional data could confirm the nature of this object as either a black hole or a B-type main-sequence star that was not direcly detected yet. If the companion were a B-type star, it would explain the third light contribution found by the 2021 publication but not the apparent non-detection in the spectrum.{{cite journal |last1=Xiao |first1=Guang-Yao |last2=Feng |first2=Fabo |last3=Wang |first3=Song |last4=Li |first4=Kai |last5=Rui |first5=Yicheng |last6=Duan |first6=Xiao-Wei |title=Detection of dark companions via the combination of eclipse timing variation, Hipparcos and/Or Gaia astrometry: The cases of V Puppis and CY Ari |date=2025 |journal=The Astrophysical Journal |arxiv=2512.20087}} If V Puppis were confirmed to harbour a black hole, it would be among the [[list of nearest known black holes|closest-known]], with a similar distance to the current leader, [[Gaia BH1]].

However, a 2026 study analysing more eclipse data found that the variations are well-explained by two orbiting stars, with the inner star matching the orbital period, semi-major axis and mass of the companion found by the 2025 study. The expected luminosity of these stars match the third-light contribution found in the 2021 publication, confirming that they are B-type stars.{{Cite journal |last=Li |first=Fu-Xing |last2=Qian |first2=Sheng-Bang |last3=Fernández Lajús |first3=Eduardo |last4=Li |first4=Lin-Jia |last5=Zhao |first5=Er-Gang |last6=Zhu |first6=Li-Ying |last7=Jiao |first7=Cheng-Liang |last8=Sun |first8=Qi-Bin |last9=Lin |first9=Wen-Xu |last10=Liao |first10=Wen-Ping |last11=Shi |first11=Xiang-Dong |last12=Li |first12=Min-Yu |date=2026-04-20 |title=V Pup: A Hierarchical Massive Quadruple System |journal=The Astrophysical Journal |volume=1001 |issue=2 |pages=183 |doi=10.3847/1538-4357/ae4de8 |issn=0004-637X}}

However, a 2026 study analysing more eclipse data found that the variations are well-explained by two orbiting stars, with the inner star matching the orbital period, semi-major axis and mass of the companion found by the 2025 study. The expected luminosity of these stars match the third-light contribution found in the 2021 publication, confirming that they are B-type stars.{{Cite journal |last1=Li |first1=Fu-Xing |last2=Qian |first2=Sheng-Bang |last3=Fernández Lajús |first3=Eduardo |last4=Li |first4=Lin-Jia |last5=Zhao |first5=Er-Gang |last6=Zhu |first6=Li-Ying |last7=Jiao |first7=Cheng-Liang |last8=Sun |first8=Qi-Bin |last9=Lin |first9=Wen-Xu |last10=Liao |first10=Wen-Ping |last11=Shi |first11=Xiang-Dong |last12=Li |first12=Min-Yu |date=2026-04-20 |title=V Pup: A Hierarchical Massive Quadruple System |journal=The Astrophysical Journal |volume=1001 |issue=2 |pages=183 |doi=10.3847/1538-4357/ae4de8 |doi-access=free |issn=0004-637X}}

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==Further reading==

==Further reading==

*{{Cite journal |last=Andersen |first=J. |last2=Clausen |first2=J. V. |last3=Gimenez |first3=A. |last4=Nordstroem |first4=B. |date=December 1983 |title=Absolute dimensions of eclipsing binaries. II. The early-type semidetached system V Puppis. |bibcode=1983A&A...128...17A |journal=Astronomy and Astrophysics |language=en |volume=128 |pages=17–28 |issn=0004-6361}}

*{{Cite journal |last1=Andersen |first1=J. |last2=Clausen |first2=J. V. |last3=Gimenez |first3=A. |last4=Nordstroem |first4=B. |date=December 1983 |title=Absolute dimensions of eclipsing binaries. II. The early-type semidetached system V Puppis. |bibcode=1983A&A...128...17A |journal=Astronomy and Astrophysics |language=en |volume=128 |pages=17–28 |issn=0004-6361}}

*{{Cite journal |last=Stickland |first=D. J. |last2=Lloyd |first2=C. |last3=Pachoulakis |first3=I. |last4=Koch |first4=R. H. |date=December 1998 |title=Spectroscopic binary orbits from ultraviolet radial velocities. Paper 29: V Puppis (HD 65818) |journal=The Observatory |language=en |volume=118 |pages=356–364 |bibcode=1998Obs...118..356S |issn=0029-7704}}

*{{Cite journal |last1=Stickland |first1=D. J. |last2=Lloyd |first2=C. |last3=Pachoulakis |first3=I. |last4=Koch |first4=R. H. |date=December 1998 |title=Spectroscopic binary orbits from ultraviolet radial velocities. Paper 29: V Puppis (HD 65818) |journal=The Observatory |language=en |volume=118 |pages=356–364 |bibcode=1998Obs...118..356S |issn=0029-7704}}

{{Stars of Puppis}}

{{Stars of Puppis}}