V728 Scorpii

In this article, we will explore the topic of V728 Scorpii in depth, analyzing its many facets and its impact on different aspects of daily life. From its origins to its relevance today, we will immerse ourselves in a journey through the history, advances, challenges and opportunities that V728 Scorpii presents in society. Through different perspectives, we will address its influence on culture, the economy, technology and interpersonal relationships, with the aim of fully understanding its importance and the implications it entails. Likewise, we will examine the different points of view and opinions of experts in the field, in order to offer a broad and complete vision about V728 Scorpii. Join us on this exciting journey to discover everything V728 Scorpii has to offer!

V728 Scorpii
Location of V728 Scorpii (circled in red)
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 17h 39m 13.239s[1]
Declination −45° 28′ 45.68″[1]
Apparent magnitude (V) 5.0 - 21[2]
Characteristics
Variable type Nova and eclipsing[2]
Astrometry
Proper motion (μ) RA: −9.805[1] mas/yr
Dec.: −13.978[1] mas/yr
Parallax (π)0.4761±0.1257 mas[1]
Distanceapprox. 7,000 ly
(approx. 2,100 pc)
Other designations
Nova Sco 1862, Gaia DR2 5949183467703297920, AAVSO 1731-45[3]
Database references
SIMBADdata

V728 Scorpii, also known as Nova Scorpii 1862, was a nova that occurred in the constellation of Scorpius. It was discovered on 4 October 1862 by John Tebbutt, an astronomer living in New South Wales, Australia, while observing a comet. He reported that the star was in the constellation Ara.[4] At the time of its discovery, the nova had an apparent magnitude of 5, making it visible to the unaided eye. Nine days later, it faded below 11th magnitude, indicating that it was a very fast nova.[5]

A visual band light curve for V728 Scorpii. The main plot shows the long-term variation with arrows pointing to the stunted outbursts which occur every ~30 days. The inset plot shows the variation caused by the eclipses. Adapted from Vogt et al. (2018)[6] and Tappert et al. (2013).[7]

Tappert et al. conducted an observing program from 2009 to 2011 to investigate nova candidates. Using photometric and spectroscopic observations, they identified the post-nova star corresponding to Nova Scorpii 1862. On 20 May 2009, the star had a visible-band magnitude of 18.5. They reported that the spectrum resembled that of a dwarf nova with a high orbital inclination, suggesting that it might be an eclipsing variable.[8] Follow-up observations by the same team found that V728 Scorpii was indeed an eclipsing system. All novae are binary stars, in a very close orbit with a "donor" star transferring material to a white dwarf companion. The eclipses in this system appear to be eclipses of the accretion disk surrounding the white dwarf, rather than either star. The orbital period is 3.32 hours.[7]

References

  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. ^ a b "V728 Sco". International Variable Star Index. Retrieved 2020-12-31.
  3. ^ "V728 Scorpii". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-11.
  4. ^ Tebbutt, J. (March 1878). "On a New Variable in the Constellation Ara". Monthly Notices of the Royal Astronomical Society. 38 (5): 330–331. Bibcode:1878MNRAS..38..330T. doi:10.1093/mnras/38.5.330.
  5. ^ Duerbeck, Hilmar W. (March 1987). "A Reference Catalogue and Atlas of Galactic Novae". Space Science Reviews. 45 (1–2): 1–14. Bibcode:1987SSRv...45....1D. doi:10.1007/BF00187826. S2CID 115854775.
  6. ^ Vogt, N.; Tappert, C.; Puebla, E. C.; Fuentes-Morales, I. (August 2018). "Life after eruption – VII. A search for stunted outbursts in 13 post-novae". Monthly Notices of the Royal Astronomical Society. 478 (4): 5427–5435. Bibcode:2018MNRAS.478.5427V. doi:10.1093/mnras/sty1445.
  7. ^ a b Tappert, C.; Vogt, N.; Schmidtobreick, L.; Ederoclite, A.; Vanderbeke, J. (May 2013). "Life after eruption - II. The eclipsing old nova V728 Scorpii". Monthly Notices of the Royal Astronomical Society. 431 (1): 92–101. arXiv:1302.5570. Bibcode:2013MNRAS.431...92T. doi:10.1093/mnras/stt139.
  8. ^ Tappert, C.; Ederoclite, A.; Mennickent, R.E.; Schmidtobreick, L.; Vogt, N. (July 2012). "Life after eruption - I. Spectroscopic observations of 10 nova candidates". Monthly Notices of the Royal Astronomical Society. 423 (3): 2476–2485. arXiv:1204.1501. Bibcode:2012MNRAS.423.2476T. doi:10.1111/j.1365-2966.2012.21054.x.