V4046 Sagittarii

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V4046 Sagittarii
V4046SgrLightCurve.png
A blue band light curve for V4046 Sagittarii, adapted from Quast et al. (2000) [1]
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
HD  319139, CD −32° 13906, GSC  07396-00644
Database references
SIMBAD data

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]

Contents

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 74 exocomet belts imaged by ALMA's REASONS survey, showing belts of all shapes, sizes and ages (REASONS comboplot full nonames).jpg
Image of the disk around the red dwarf GSC 07396-00759 from the REASONS survey [7]

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. [8] GSC 07396-00759 itself has an edge-on debris disk with a radius of 70 au, [9] and may be a binary as well, making V4046 Sagittarii a potentially quadruple system. [8]

See also

Related Research Articles

<span class="mw-page-title-main">Protoplanetary disk</span> Gas and dust surrounding a newly formed star

A protoplanetary disk is a rotating circumstellar disc of dense gas and dust surrounding a young newly formed star, a T Tauri star, or Herbig Ae/Be star. The protoplanetary disk may not be considered an accretion disk; while the two are similar, an accretion disk is hotter and spins much faster. It is also found on black holes, not stars. This process should not be confused with the accretion process thought to build up the planets themselves. Externally illuminated photo-evaporating protoplanetary disks are called proplyds.

<span class="mw-page-title-main">Upsilon Sagittarii</span> Binary star system in the constellation Sagittarius

Upsilon Sagittarii is a spectroscopic binary star system in the constellation Sagittarius. Upsilon Sagittarii is the prototypical hydrogen-deficient binary (HdB), and one of only four such systems known. The unusual spectrum of hydrogen-deficient binaries has made stellar classification of Upsilon Sagittarii difficult.

<span class="mw-page-title-main">TW Hydrae</span> T Tauri star in the constellation Hydra

TW Hydrae is a T Tauri star approximately 196 light-years away in the constellation of Hydra. TW Hydrae is about 80% of the mass of the Sun, but is only about 5-10 million years old. The star appears to be accreting from a protoplanetary disk of dust and gas, oriented face-on to Earth, which has been resolved in images from the ALMA observatory. TW Hydrae is accompanied by about twenty other low-mass stars with similar ages and spatial motions, comprising the "TW Hydrae association" or TWA, one of the closest regions of recent "fossil" star-formation to the Sun.

HD 98800, also catalogued as TV Crateris, is a quadruple star system in the constellation of Crater. Parallax measurements made by the Hipparcos spacecraft put it at a distance of about 150 light-years away. The system is located within the TW Hydrae association (TWA), and has received the designation TWA 4.

<span class="mw-page-title-main">9 Sagittarii</span> Star in the constellation Sagittarius

9 Sagittarii is a massive binary star in the constellation Sagittarius. It has an apparent magnitude of 5.97. Both components are highly luminous O-type main-sequence stars.

<span class="mw-page-title-main">GG Tauri</span> Star in the constellation Taurus

GG Tauri, often abbreviated as GG Tau, is a quintuple star system in the constellation Taurus. At a distance of about 450 light years away, it is located within the Taurus-Auriga Star Forming Region. The system comprises three stars orbiting each other in a hierarchical triple system, known as GG Tauri A, and another binary star system more distant from the central system, known as GG Tauri B.

<span class="mw-page-title-main">KH 15D</span> Binary star system in the constellation Monoceros

KH 15D, described as a winking star because of its unusual dips in brightness, is a binary T Tauri star system embedded in a circumbinary disk. It is a member of the young open cluster NGC 2264, located about 2,500 light-years (770 pc) from the Sun in the constellation of Monoceros.

<span class="mw-page-title-main">Circumplanetary disk</span> Accumulation of matter around a planet

A circumplanetary disk is a torus, pancake or ring-shaped accumulation of matter composed of gas, dust, planetesimals, asteroids or collision fragments in orbit around a planet. They are reservoirs of material out of which moons may form. Such a disk can manifest itself in various ways.

<span class="mw-page-title-main">DH Tauri</span> Star in the constellation Taurus

DH Tauri, also known as DH Tau, is a type M star, located 140 parsecs away. It forms a binary system with DI Tauri 15″ away, and has a substellar companion, either a brown dwarf or massive exoplanet.

<span class="mw-page-title-main">AK Scorpii</span> Binary star in the constellation Scorpius

AK Scorpii is a Herbig Ae/Be star and spectroscopic binary star about 459 light-years distant in the constellation Scorpius. The star belongs to the nearby Upper Centaurus–Lupus star-forming region and the star is actively accreting material. The binary is surrounded by a circumbinary disk that was imaged with VLT/SPHERE in scattered light and with ALMA.

<span class="mw-page-title-main">ROXs 12</span>

ROXs 12 is a binary system of pre-main-sequence stars. It belongs to the Rho Ophiuchi cloud complex. The surface temperature of the primary star is 3900±100 K. ROXs 12 is much younger than the Sun with an age of 7.6+4.1
−2.5 million years.

<span class="mw-page-title-main">RW Aurigae</span> Young binary star system in the constellation Auriga

RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away, belonging to the Taurus-Auriga association of the Taurus Molecular Cloud. RW Aurigae B was discovered in 1944.

<span class="mw-page-title-main">HK Tauri</span> Young binary star system in the constellation of Taurus

HK Tauri is a young binary star system in the constellation of Taurus about 434 light-years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">GI Tauri and GK Tauri</span> Binary star system in the constellation of Taurus

GK Tauri is a young T Tauri-type pre-main sequence star in the constellation of Taurus about 421 light years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">GV Tauri</span> Young binary star system in the constellation of Taurus

GK Tauri is a young binary system composed of T Tauri-type pre-main sequence stars in the constellation of Taurus about 466 light years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">DL Tauri</span> Protostar system with planetary system in the constellation of Taurus

DL Tauri is a young T Tauri-type pre-main sequence stars in the constellation of Taurus about 522 light years away, belonging to the Taurus Molecular Cloud. It is partially obscured by the foreground gas cloud rich in carbon monoxide, and is still accreting mass, producing 0.14 L☉ due to release of accretion energy. The stellar spectrum shows the lines of ionized oxygen, nitrogen, sulfur and iron.

<span class="mw-page-title-main">V4332 Sagittarii</span>

V4332 Sagittarii is a nova-like event in the constellation of Sagittarius. It was discovered on February 24, 1994 at an apparent visual magnitude of 8.9 by Japanese amateur astronomer Minoru Yamamoto from Okazaki, Aichi, then confirmed by K. Hirosawa. Initially designated Nova Sagittarii 1994 #1, it was given the variable star designation V4332 Sgr. A spectra of the event taken on March 4 lacked the characteristic features of a classical nova, with the only emission lines being of the Balmer series. Subsequent spectra showed a rapid decline in luminosity and a change of spectral type over a period of five days. By 2003, the object was ~1500 times less luminous than at peak magnitude and showed a spectrum of an M-type star.

<span class="mw-page-title-main">RS Sagittarii</span> Eclipsing binary star system in the constellation Sagittarius

RS Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated RS Sgr. It is a double-lined spectroscopic binary with an orbital period of 2.416 days, indicating that the components are too close to each other to be individually resolved. The system has a combined apparent visual magnitude of 6.01, which is bright enough to be faintly visible to the naked eye. During the primary eclipse the brightness drops to magnitude 6.97, while the secondary eclipse is of magnitude 6.28. The distance to this system is approximately 1,420 light years based on parallax measurements.

<span class="mw-page-title-main">V356 Sagittarii</span> Star system in the constellation Sagittarius

V356 Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated V356 Sgr. It has a peak apparent visual magnitude of 6.84, which decreases to 7.66 during the primary eclipse and 7.24 with the secondary eclipse. Based on parallax measurements, this system is located at a distance of approximately 2,210 light years from the Sun.

References

  1. ↑ 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: 28. Bibcode:2000IAUS..200P..28Q . Retrieved 10 March 2022.
  2. 1 2 Høg, E. (1998). "The Tycho Reference Catalogue". Astronomy and Astrophysics. 335: L65. Bibcode:1998A&A...335L..65H.
  3. ↑ 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.
  4. 1 2 3 4 5 6 7 8 9 10 11 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 .
  5. 1 2 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.
  6. ↑ 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. 510: 1248–1257. arXiv: 2111.12668 . doi: 10.1093/mnras/stab3440 .
  7. ↑ Matrà, L.; Marino, S.; Wilner, D. J.; Kennedy, G. M.; Booth, M.; Krivov, A. V.; Williams, J. P.; Hughes, A. M.; Burgo, C. del (2025-01-15). "REsolved ALMA and SMA Observations of Nearby Stars (REASONS): A population of 74 resolved planetesimal belts at millimetre wavelengths". arXiv: 2501.09058 [astro-ph].
  8. 1 2 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.
  9. ↑ 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. arXiv: 2202.11711 . doi: 10.1093/mnras/stac536 .
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