RW Aurigae

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Coordinates: Sky map 05h 07m 49.4561s, +30° 24′ 04.7772″

RW Aurigae
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
RW Aurigae A
Right ascension 05h 07m 49.4561s[1]
Declination +30° 24′ 04.7772″[1]
Apparent magnitude (V) 9.6
RW Aurigae B
Right ascension 05h 07m 49.5652s[2]
Declination 30° 24′ 05.1361″[2]
Apparent magnitude (V)
Characteristics
RW Aurigae A
Spectral type K1-K3[3]
Apparent magnitude (G) 12.2048±0.0093[4]
Variable type T Tau
RW Aurigae B
Spectral type K5[3]
Apparent magnitude (G) 13.3177±0.0653[5]
Astrometry
A
Proper motion (μ) RA: 2.747[1] mas/yr
Dec.: -27.558[1] mas/yr
Parallax (π)6.1157 ± 0.0665[4] mas
Distance533 ± 6 ly
(164 ± 2 pc)
B
Proper motion (μ) RA: 4.238[2] mas/yr
Dec.: -24.996[2] mas/yr
Parallax (π)6.5835 ± 0.9023[5] mas
Distanceapprox. 500 ly
(approx. 150 pc)
Position (relative to RW Aurigae A)[6]
ComponentRW Aurigae B
Epoch of observation4/6/2007
Angular distance1.448±0.005″
Position angle255.9±0.3°
Observed separation
(projected)		237 AU
Details
A
Mass1.34±0.18[3] M☉
Luminosity0.59[3] L☉
Temperature5082[3] K
Rotation5.6 d.[7]
Age3±1[8] Myr
B
Mass0.9[9] M☉
Radius1.5[8] R☉
Luminosity0.6[8] L☉
Temperature4150±50[8] K
Age3±1[8] Myr
Other designations
BD+30 792, HD 240764, HIP 23873, TYC 2389-955-1, GSC 02389-00955, 2MASS J05074953+3024050
RW Aurigae A: Gaia DR2 156430822114424576
RW Aurigae B: Gaia DR2 156430817820015232
Database references
SIMBADdata

RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away, belonging to the of the Taurus Molecular Cloud. RW Aurigae B was discovered in 1944.[6]

System[]

The two stars of the RW Aurigae system are separated by 1.448″, equivalent to 237 AU at the distance of RW Aurigae. The primary is a pre-main sequence star with a mass of 1.4 M☉, while the secondary has a mass of 0.9 M☉. These are loosely bound,[8] and their orbital trajectory is nearly parabolic,[9] with an orbital period of 1000−1500 years as evidenced by the structure of the ejected dust jets. The star system's orbit is retrograde compared to the rotation direction of the disk orbiting the primary star.[6] RW Aurigae A is also suspected to be a close binary since 1999.[10]

Properties[]

Both members of the binary are medium-mass objects still contracting towards the main sequence and accreting mass, RW Aurigae A at the rate of 0.1M☉/Myr,[9] and RW Aurigae B at the rate of 0.005M☉/Myr.[8] Their ages are equal to 3±1 million years.[8]

The binary is surrounded by a complex accretion structure, containing a circumbinary shell, spiral arms, bow shocks and protoplanetary disks. The primary star is producing complex bipolar jets extending as far as 46 thousand AU from the star.[6] The protoplanetary disk of RW Aurigae A is inclined to the line of sight by 45-60 degrees.[11] It is not known if planetary formation in the disk has been arrested by stellar encounter or accelerated, as a wide range of debris sizes, consistent with both a collision cascade and ongoing planetesimal formation were detected.[12]

Variability[]

RW Aurigae A varies in brightness. It is a T Tauri variable, and a prototype for the eponymous class of a ,[citation needed] exhibiting irregular dips in its light curve due to the rapidly changing geometry of the protoplanetary disk, disturbed by the periastron passage of RW Aurigae B.[9]A previous periastron passage happened about 400 years ago.[8] The long-lasting brightness dips in 2010-2011 and 2014-2016 have reduced the star's brightness to magnitude12.5,[11] before recovering to 10.5-11.0 visual magnitude by August 2016.[13]

The companion star is itself a variable of UX Orionis type, exhibiting both chaotic variations of brightness and short (less than one day) brightness dips due to continuing accretion and the inhomogeneity of the protoplanetary disk.[8]

See also[]

References[]

  1. ^ Jump up to: a b c d "V* RW Aur A". SIMBAD. Centre de données astronomiques de Strasbourg.
  2. ^ Jump up to: a b c d "V* RW Aur B". SIMBAD. Centre de données astronomiques de Strasbourg.
  3. ^ Jump up to: a b c d e Skinner, Stephen L.; Guedel, Manuel (2014), Chandra Resolves the T Tauri Binary System RW Aur, arXiv:1404.2631
  4. ^ Jump up to: a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  5. ^ Jump up to: a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  6. ^ Jump up to: a b c d Bisikalo, D. V.; Dodin, A. V.; Kaigorodov, P. V.; Lamzin, S. A.; Malogolovets, E. V.; Fateeva, A. M. (2012), "Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model", Astronomy Reports, 56 (9): 686–692, arXiv:1207.4022, Bibcode:2012ARep...56..686B, doi:10.1134/S1063772912090028, S2CID 18483219
  7. ^ Dodin, A. V.; Lamzin, S. A.; Chountonov, G. A. (2011), "Magnetic field of young star RW Aur", Magnetic Stars: 229, arXiv:1111.2309, Bibcode:2011mast.conf..229D
  8. ^ Jump up to: a b c d e f g h i j Dodin, A.; Lamzin, S.; Petrov, P.; Safonov, B.; Takami, M.; Tatarnikov, A. (2020), "RW Aur B: A modest UX Ori-type companion of the famous primary", Monthly Notices of the Royal Astronomical Society, 497 (4): 4322–4332, arXiv:2007.12559, doi:10.1093/mnras/staa2206
  9. ^ Jump up to: a b c d Cuello, Nicolás; Louvet, Fabien; Mentiplay, Daniel; Pinte, Christophe; Price, Daniel J.; Winter, Andrew J.; Nealon, Rebecca; Ménard, François; Lodato, Giuseppe; Dipierro, Giovanni; Christiaens, Valentin; Montesinos, Matías; Cuadra, Jorge; Laibe, Guillaume; Cieza, Lucas; Dong, Ruobing; Alexander, Richard (2020), "Flybys in protoplanetary discs – II. Observational signatures", Monthly Notices of the Royal Astronomical Society, 491: 504–514, arXiv:1910.06822, doi:10.1093/mnras/stz2938
  10. ^ Gahm, G. F.; Petrov, P. P.; Duemmler, R.; Gameiro, J. F.; Lago, M. T. V. T. (1999), "RW Aur A, a close binary?", Astronomy and Astrophysics, 352: L95, Bibcode:1999A&A...352L..95G
  11. ^ Jump up to: a b Bozhinova, I.; Scholz, A.; Costigan, G.; Lux, O.; Davis, C. J.; Ray, T.; Boardman, N. F.; Hay, K. L.; Hewlett, T.; Hodosán, G.; Morton, B. (2016), "The disappearing act: A dusty wind eclipsing RW Aur", Monthly Notices of the Royal Astronomical Society, 463 (4): 4459–4468, arXiv:1609.05667, doi:10.1093/mnras/stw2327
  12. ^ Rodriguez, Joseph E.; Reed, Phillip A.; Siverd, Robert J.; Pepper, Joshua; Stassun, Keivan G.; Gaudi, B. Scott; Weintraub, David A.; Beatty, Thomas G.; Lund, Michael B.; Stevens, Daniel J. (2016), "Recurring Occultations of Rw Aurigae by Coagulated Dust in the Tidally Disrupted Circumstellar Disk", The Astronomical Journal, 151 (2): 29, arXiv:1512.03745, Bibcode:2016AJ....151...29R, doi:10.3847/0004-6256/151/2/29, S2CID 118540299
  13. ^ Scholz, Aleks; Bozhinova, Inna; Lux, Oliver; Pannicke, Anna; Mugrauer, Markus (2016). "Re-brightening of the young star RW Aur: The end of the second deep eclipse". The Astronomer's Telegram. 9428: 1. Bibcode:2016ATel.9428....1S.


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