astro.wikisort.org - Star
V4046 Sagittarii is a young binary consisting of two K-type main-sequence stars. The two stars are about 271 light-years (83 parsecs) away from the Earth.[4] The two stars orbit each other every 2.42 days on a circular orbit.[4]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 14m 10.4660s[2] |
| Declination | −32° 47′ 34.496″[2] |
| Apparent magnitude (V) | 10.68[3] |
| Characteristics | |
| Spectral type | K5Ve / K7Ve[4] |
| Variable type | T Tauri[4] |
| Astrometry | |
| Radial velocity (Rv) | −6.94[4] km/s |
| Distance | 271 ly (83[4] pc) |
| Orbit[4] | |
| Period (P) | 2.4213305(40) d |
| Semi-major axis (a) | 9.24 R☉ |
| Eccentricity (e) | ≤0.01 |
| Inclination (i) | 35° |
| Periastron epoch (T) | JD 2452380.867 ± 0.03 |
| Details | |
| Mass | 0.912 / 0.873[4] M☉ |
| Surface gravity (log g) | 4.0 / 4.0[4] cgs |
| Temperature | 4370 / 4100[4] K |
| Rotational velocity (v sin i) | 14.2 / 13.7[4] km/s |
| Age | ~12[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
V4046 Sagittarii is surrounded by a massive protoplanetary disk. The disk has a radius of about 370 astronomical units (au) with about 40 Earth masses of dust in the disk. There are two bright inner rings at 14 and 25 au from the center, respectively.[6] V4046 Sagittarii is one of four pre-main-sequence star systems within 100 parsecs with protoplanetary disks, the others being TW Hydrae, HD 141569, and 49 Ceti. The two stars are still accreting matter from the disk, and gas giant planets may be forming in the disk as well.[5]
The red dwarf GSC 07396-00759 is separated about 2.82″ from V4046 Sagittarii. Since it has a similar motion throughout space with V4046 Sagittarii, GSC 07396-00759 is assumed to be gravitationally bound (although weakly) to V4046 Sagittarii. The two systems are separated by at least 12,350 astronomical units (0.1953 ly) away, and the orbital period would be on the order of 100,000 years.[7] GSC 07396-00759 itself has an edge-on debris disk with a radius of 70 au,[8] and may be a binary as well, making V4046 Sagittarii a potentially quadruple system.[7]
See also
References
- Quast, Germano R.; Torres, Carlos A. O.; de La Reza, Ramiro; da Silva, Licio; Mayor, Michel (January 2000). "V4046 Sgr, a key young binary system". IAU Symposium 200. 200. Retrieved 10 March 2022.
- Høg, E. (1998). "The Tycho Reference Catalogue". Astronomy and Astrophysics. 335: L65. Bibcode:1998A&A...335L..65H.
- Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
- Stempels, H. C.; Gahm, G. F. (2004). "The close T Tauri binary V 4046 Sagittarii". Astronomy & Astrophysics. 421 (3): 1159. Bibcode:2004A&A...421.1159S. doi:10.1051/0004-6361:20034502.
- Rodriguez, David R.; Kastner, Joel H.; Wilner, David; Qi, Chunhua (2010). "Imaging the Molecular Disk Orbiting the Twin Young Suns of V4046 Sgr". The Astrophysical Journal. 720 (2): 1684. arXiv:1007.3993. Bibcode:2010ApJ...720.1684R. doi:10.1088/0004-637X/720/2/1684. S2CID 118379005.
- Martinez–Brunner, Rafael; Casassus, Simon; Pérez, Sebastián; Hales, Antonio; Weber, Philipp; Carcamo, Miguel; Arce-Tord, Carla; Cieza, Lucas; Garufi, Antonio; Marino, Sebastián; Zurlo, Alice (2021). "High-resolution ALMA observations of V4046 Sgr: A circumbinary disc with a thin ring". Monthly Notices of the Royal Astronomical Society. arXiv:2111.12668. doi:10.1093/mnras/stab3440.
- Kastner, J. H.; Sacco, G. G.; Montez, R.; Huenemoerder, D. P.; Shi, H.; Alecian, E.; Argiroffi, C.; Audard, M.; Bouvier, J.; Damiani, F.; Donati, J.-F.; Gregory, S. G.; Güdel, M.; Hussain, G. A. J.; Maggio, A.; Montmerle, T. (2011). "GSC 07396-00759 = V4046 Sgr C[D]: A Wide-separation Companion to the Close T Tauri Binary System V4046 Sgr AB". The Astrophysical Journal. 740 (1): L17. arXiv:1109.3389. Bibcode:2011ApJ...740L..17K. doi:10.1088/2041-8205/740/1/L17. S2CID 14660453.
- Cronin-Coltsmann, Patrick F.; Kennedy, Grant M.; Adam, Christian; Kral, Quentin; Lestrade, Jean-François; Marino, Sebastian; Matrà, Luca; Murphy, Simon J.; Olofsson, Johan; Wyatt, Mark C. (2022). "ALMA's view of the M-dwarf GSC 07396-00759's edge-on debris disc: AU Mic's coeval twin". Monthly Notices of the Royal Astronomical Society. 512 (4): 4752–4764. doi:10.1093/mnras/stac536.
External links
- "V4046 Sagittarii". Retrieved 2010-10-06.
- Huang, Jane; Öberg, Karin I.; Qi, Chunhua; Aikawa, Yuri; Andrews, Sean M.; Furuya, Kenji; Guzmán, Viviana V.; Loomis, Ryan A.; Van Dishoeck, Ewine F.; Wilner, David J. (2017). "An ALMA Survey of DCN/H13CN and DCO+/H13CO+ in Protoplanetary Disks". The Astrophysical Journal. 835 (2): 231. arXiv:1701.01735. Bibcode:2017ApJ...835..231H. doi:10.3847/1538-4357/835/2/231. S2CID 54805047.
На других языках
[de] V4046 Sagittarii
V4046 Sagittarii, kurz V4046 Sgr, ist ein etwa 240 Lichtjahre entferntes spektroskopisches Doppelsternsystem im Sternbild Schütze. Die Komponenten gehören den Spektralklassen K5 und K7 an und haben fast identische Massen von je etwa 0,9 Sonnenmassen; sie sind nur wenige Sonnenradien voneinander entfernt. Ihr Alter beträgt etwa 12 Millionen Jahre. Im Juni 2009 konnte mit Hilfe des Submillimeter-Array-Radioteleskops eine die Sterne umgebene protoplanetare Scheibe nachgewiesen werden. Dies war die erste Entdeckung solch einer Scheibe in einem Doppelsternsystem und V4046 Sgr ist das bisher älteste Sternensystem in dem solch eine Scheibe nachgewiesen wurde.[1]- [en] V4046 Sagittarii
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