Astronomy:V1094 Scorpii
250px Visual band light curves for V1094 Scorpii, adapted from Wichmann et al. (1998)[2] and Joergens et al. (2001)[3] | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Lupus |
| Right ascension | 16h 08m 36.17701s[4] |
| Declination | −39° 23′ 02.4621″[4] |
| Apparent magnitude (V) | 13.48 |
| Characteristics | |
| Spectral type | K6V[5] |
| Variable type | T Tauri-type |
| Astrometry | |
| Proper motion (μ) | RA: −9.830[4] mas/yr Dec.: +23.435[4] mas/yr |
| Parallax (π) | 6.5086 ± 0.0452[4] mas |
| Distance | 501 ± 3 ly (154 ± 1 pc) |
| Details[1] | |
| Mass | 0.88 M☉ |
| Radius | 1.6 R☉ |
| Luminosity | 0.64 L☉ |
| Temperature | 4,116 K |
| Age | 2.4 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
V1094 Scorpii is a young stellar object in the constellation of Scorpius, located in the young Lupus Star Forming Region.[6] It is being orbited by a protoplanetary disk that extends out to a distance of 300 astronomical unit|AU from the host star. There are gaps at 100 AU and 170 AU, with bright rings at 130 AU and 220 AU.[5]
A 2026 study analyzed ALMA Band 6 (1.3 mm) continuum and CO line data together with a VLT/SPHERE near-infrared scattered-light image, using 2D super-resolution imaging to resolve the disk at higher angular resolution. It found four narrow dust ring–gap pairs, with the dust continuum extending to about 380 AU and the CO gas disk extending to roughly 760 AU in Keplerian rotation, placing V1094 Sco among the largest known Class II disks.[1] The same work derived a dynamical stellar mass of about 0.88 M☉ and inferred weak turbulence in the outer disk. The authors interpreted the substructure as having a hybrid origin: a low-mass companion of about 55 Earth masses near 100 AU driving the inner double gap, and secular gravitational instability producing the outer rings at 170–230 AU.[1]
In 1998, Rainer Wichmann et al. announced that the star, then known as RXJ1608.6-3922, is a variable star, based on visual band photometry over a nine day interval. They classified it as an eclipsing binary.[7] Later observations showed that the brightness variations are due to starspots.[3] It was given its variable star designation in the year 2000.[8]
Periodic radial velocity variations in the young star V1094 Scorpii had at first been explained by the presence of a substellar object in a tight orbit.[9] Currently, the presence of a substellar object has been retracted; again starspots have been invoked as the actual cause for observed radial velocity variations.[3]
References
- ↑ 1.0 1.1 1.2 1.3 Yamaguchi, Masayuki et al. (2026). "A Hybrid Origin for the Multiple Ring-Gap Structures in the Large Protoplanetary Disk V1094 Sco: A Low-Mass Planet and Secular Gravitational Instability". The Astrophysical Journal. Bibcode: 2026arXiv260511486Y.
- ↑ Wichmann, R.; Bouvier, J.; Allain, S.; Krautter, J. (February 1998). "Rotational evolution of pre-main sequence stars in Lupus". Astronomy and Astrophysics 330: 521–532. Bibcode: 1998A&A...330..521W. https://ui.adsabs.harvard.edu/abs/1998A&A...330..521W. Retrieved 19 March 2022.
- ↑ 3.0 3.1 3.2 Joergens, V. et al. (2001). "The T Tauri star RX J1608.6-3922 - not an eclipsing binary but a spotted single star". Astronomy and Astrophysics 373 (3): 966–973. doi:10.1051/0004-6361:20010684. Bibcode: 2001A&A...373..966J.
- ↑ 4.0 4.1 4.2 4.3 4.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 5.0 5.1 van Terwisga, S. E. et al. (August 2018). "V1094 Scorpii: A rare giant multi-ringed disk around a T Tauri star". Astronomy & Astrophysics 616: 10. doi:10.1051/0004-6361/201832862. A88. Bibcode: 2018A&A...616A..88V.
- ↑ Hughes, Joanne et al. (1993). "The distance to the Lupus star formation region". The Astronomical Journal 105 (2): 571–575. doi:10.1086/116454. Bibcode: 1993AJ....105..571H.
- ↑ Wichmann, R.; Bouvier, J.; Allain, S.; Krautter, J. (February 1998). "Rotational evolution of pre-main sequence stars in Lupus". Astronomy and Astrophysics 330: 521-532. Bibcode: 1998A&A...330..521W. https://articles.adsabs.harvard.edu/pdf/1998A%26A...330..521W. Retrieved 15 September 2025.
- ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V. (March 2000). "The 75th Name-List of Variable Stars". Information Bulletin on Variable Stars 4870: 1-47. Bibcode: 2000IBVS.4870....1K. https://ibvs.konkoly.hu/pub/ibvs/4801/4870.pdf. Retrieved 15 September 2025.
- ↑ Wichmann, R. et al. (1997). "T Tauri stars and the Gould Belt near Lupus". Astronomy and Astrophysics 326: 211–217. Bibcode: 1997A&A...326..211W.
 |  |
