Gliese 752

Gliese 752
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila
Gliese 752 A
Right ascension 19h 16m 55.257s[1]
Declination +05° 10′ 08.05″[1]
Apparent magnitude (V) ~9.13[1]
Gliese 752 B
Right ascension 19h 16m 57.62s[2]
Declination +05° 09′ 02.2″[2]
Apparent magnitude (V) ~17.30[2]
Characteristics
Spectral type M2.5[1] / M8V[2]
Apparent magnitude (B) ~10.63[1] / ~19.42[2]
Apparent magnitude (V) ~9.13[1] / ~17.30[2]
Apparent magnitude (R) ~8.3[1] / ~15.6[2]
Apparent magnitude (J) ~5.58[1] / 9.908 ±0.025[2]
Apparent magnitude (H) ~4.93[1] / 9.226 ±0.026[2]
Apparent magnitude (K) ~4.67[1] / 8.765 ±0.022[2]
Variable type BY[3]/UV[4]
Astrometry
Proper motion (μ) RA: −614[2] mas/yr
Dec.: −1368[2] mas/yr
Parallax (π)164.3[2] ± 3.5[2] mas
Distance18.72 ly
(5.74[5] pc)
Absolute magnitude (MV)10.13[5]/18.7[6]
Details
Mass0.46[5] / 0.075 ±.05[7] M☉
Radius0.546[5] / ~.102[5] R☉
Temperature~3240[5] / ~2600[5] K
Metallicity–0.05 ± 0.17[8]
Age? / ~1G[7] years
Other designations
Gliese 752 A[1]

2MASS J19165526+0510086, BD+04 4048 A, GSC 00472-01252, HD 180617, HIP 94761, Ross 652, TYC 472-1252-1, V1428 Aquilae, Wolf 1055

Gliese 752 B[2]
2MASS J19165762+0509021, BD+04 4048 B, V1298 Aquilae, VB 10
Database references
SIMBADThe system
A
vB 10 (B)

Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of about 19 light years.[5] This system consists of two M-type stars. The primary star is the magnitude 9 Gliese (GJ) 752 A. The secondary star is the dim magnitude 17 Gliese (GJ) 752 B, more commonly referred to as VB 10. This stellar pair form an astrometric binary star system separated by about 74 arc seconds (~434 AU).[6] This system is also known for its high proper motion of about 1 arc second a year.

The name and number are from the Catalogue of Nearby Stars, published by German astronomer Wilhelm Gliese in 1969.[9]

Distance

Gliese 752 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Woolley et al. (1970) 172±4 5.81+0.14
−0.13		 19+0.5
−0.4		 179.4+4.3
−4.1		 [10]
Gliese & Jahreiß (1991) 176.7±2.4 5.66±0.08 18.46±0.25 174.6+2.4
−2.3		 [11]
Monet et al. (1992) 170.1±0.8 5.879±0.028 19.17±0.09 181.4+0.9
−0.8
van Altena et al. (1992) 172.8±0.8 5.787±0.027 18.87±0.09 178.6±0.8
Tinney (1993) 171.7±4.0 5.82+0.14
−0.13		 19+0.5
−0.4		 179.7+4.3
−4.1
van Altena et al. (1995) 171.2±0.7 5.841±0.024 19.05±0.08 180.2±0.7 [12]
Tinney et al. (1995) 169.3±5.8 5.91+0.21
−0.2		 19.3+0.7
−0.6		 182.3+6.5
−6
Tinney (1996) 164.3±4.0[nb 1] 6.09+0.15
−0.14		 19.9±0.5 187.8+4.7
−4.5
Perryman et al. (1997) (Hipparcos) 170.26±1.37 5.87±0.05 19.16+0.16
−0.15		 181.2+1.5
−1.4		 [13]
Perryman et al. (1997) (Tycho) 158.90±19.10 6.3+0.9
−0.7		 20.5+2.8
−2.2		 194.2+26.5
−20.8		 [14]
Gould & Chaname (2004) 170.26±1.37[nb 2] 5.87±0.05 19.16+0.16
−0.15		 181.2+1.5
−1.4
van Leeuwen (2007) 170.36±1.00 5.87±0.03 19.15±0.11 181.1±1.1 [15]
Pravdo & Shaklan (2009) 171.6+1.4
−1.3		 5.83+0.04
−0.05		 19.01±0.15 179.8+1.4
−1.5		 [16]
RECONS TOP100 (2012) 170.96±0.52[nb 3] 5.849±0.018 19.08±0.06 180.5+0.6
−0.5		 [17]

Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.

Interior dynamics of the Gliese 752 stars

Diagram showing the relative sizes and internal dynamic processes of the two Gliese 752 stars.

Before the Hubble Space Telescope observation of Gliese 752 system, astronomers thought magnetic fields in stars required the same dynamo process that creates magnetic fields on the Sun. In the classic solar model heat generated by nuclear fusion reactions at the star's center escapes through a radiative zone just outside the core. The heat travels from the radiative core to the star's surface through a convection zone. In this region, heat bubbles to the surface by motions similar to boiling in a pot of water.

Dynamos, which accelerate electrons to create magnetic forces, operate when the interior of a star rotates faster than its surface. Recent studies of the Sun indicate its convection zone rotates at nearly the same rate at all depths. This means the solar dynamo must operate in the more rapidly rotating radiative core just below the convective zone.[18]

Gliese 752 A characteristics

The primary star, also known as Wolf 1055, is a type M2.5 red dwarf with about half the size and mass as the Sun and considerably cooler at 3240°K. This star was first observed to be a high proper motion star by the German astronomer Max Wolf with his pioneering use of astrophotography. He added this star to his extensive catalog of such stars in 1919.[19] It is a variable star with the variable star catalog name V1428 Aquilae. It is a BY Draconis type variable star subject to flare events.[1][3]

Gliese 752 B characteristics

Main article: VB 10

Gliese 752 was not known to be a binary star system until the discovery of a small dim secondary star by George Van Biesbroeck in 1944. This star is identified as VB 10 in Van Biesbroeck's star catalog. This star is notable for its very low mass. At .08 solar mass it is near the lower mass limit for a star. It is also quite small at 10% of the solar radius.[6]

This star is a type M8V red dwarf. This star is also known for its very low luminosity, with an absolute magnitude of nearly 19, due to its very cool surface temperature of only 2600°K.[2] It is a variable star with the variable star catalog name V1298 Aquilae. This star is a UV Ceti type variable star also subject to flare events. It shares the large proper motion, along with the tendency to flare, with the primary star.[4]

In 2009 the discovery of the extrasolar planet, VB 10b, was announced in orbit around this star.[7] However a subsequent spectrographic survey failed to confirm the presence of any large planets in orbit around this star.[20]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 1.10 1.11 "SIMBAD query result: V* V1428 Aql -- Flare Star". Centre de Données astronomiques de Strasbourg. Retrieved 2009-05-30.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 2.9 2.10 2.11 2.12 2.13 2.14 2.15 "SIMBAD query result: V* V1298 Aql -- Flare Star". Centre de Données astronomiques de Strasbourg. Retrieved 2009-05-28.
  3. ↑ 3.0 3.1 "V1428 Aql". General Catalogue of Variable Stars, Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2009-06-06.
  4. ↑ 4.0 4.1 "V1298 Aql". General Catalogue of Variable Stars, Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2009-05-28.
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Linsky, Jeffrey L.; Wood, Brian E.; Brown, Alexander; Giampapa, Mark S.; Ambruster, Carol (December 20, 1995). "Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10". The Astrophysical Journal 455: 670–676. Bibcode:1995ApJ...455..670L. doi:10.1086/176614.
  6. ↑ 6.0 6.1 6.2 van Biesbroeck, G. (August 1944). "The star of lowest known luminosity". The Astronomical Journal 51: 61–62. Bibcode:1944AJ.....51...61V. doi:10.1086/105801.
  7. ↑ 7.0 7.1 7.2 Pravdo et al. (June 2009). "An Ultracool Star's Candidate Planet" (PDF). Submitted to the Astrophysical Journal. arXiv:0906.0544. Bibcode:2009ApJ...700..623P. doi:10.1088/0004-637X/700/1/623. Retrieved 2009-05-30.arXiv:0906.0544 abstract
  8. ↑ Rojas-Ayala, Bárbara et al. (April 2012). "Metallicity and Temperature Indicators in M Dwarf K-band Spectra: Testing New and Updated Calibrations with Observations of 133 Solar Neighborhood M Dwarfs". The Astrophysical Journal 748 (2): 93. arXiv:1112.4567. Bibcode:2012ApJ...748...93R. doi:10.1088/0004-637X/748/2/93. See table 3.
  9. ↑ Gliese, W. "Catalogue of Nearby Stars. Edition 1969". Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg, Nr. 22, Verlag G. Braun, Karlsruhe, 117 Seiten. Bibcode:1969VeARI..22....1G.
  10. ↑ Woolley R.; Epps E. A.; Penston M. J.; Pocock S. B. (1970). "Woolley 752". Catalogue of stars within 25 parsecs of the Sun.
  11. ↑ Gliese, W. and Jahreiß, H. (1991). "Gl 752". Preliminary Version of the Third Catalogue of Nearby Stars.
  12. ↑ Van Altena W. F., Lee J. T., Hoffleit E. D. (1995). "GCTP 4494". The General Catalogue of Trigonometric Stellar Parallaxes (Fourth ed.).
  13. ↑ Perryman et al. (1997). "HIP 94761". The Hipparcos and Tycho Catalogues.
  14. ↑ Perryman et al. (1997). "HIP 94761". The Hipparcos and Tycho Catalogues.
  15. ↑ van Leeuwen F. (2007). "HIP 94761". Validation of the new Hipparcos reduction.
  16. ↑ Pravdo, Steven H.; Shaklan, Stuart B. (2009). "An ultracool Star's Candidate Planet". The Astrophysical Journal (IOPscience) 700 (1): 623–632. arXiv:0906.0544. Bibcode:2009ApJ...700..623P. doi:10.1088/0004-637X/700/1/623.
  17. ↑ "RECONS TOP100". THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars). 2012.
  18. ↑ "Red Dwarf Dynamo Raises Puzzle over Interiors of Lowest Mass Stars". hubblesite. 1995-01-10. Retrieved 2009-08-03.
  19. ↑ Wolf, M. (August 1919). "Starkbewegter Stern in Aquila". Astronomische Nachrichten 209: 61. Bibcode:1919AN....209...61W. doi:10.1002/asna.19192090406.
  20. ↑ Bean, Jacob; Andreas Seifahrt; Henrik Hartman; Hampus Nilsson; Ansgar Reiners; Stefan Dreizler; Henry; Guenter Wiedemann (2009). "The CRIRES Search for Planets Around the Lowest-Mass Stars. II. No Giant Planet Orbiting VB10". arXiv:0912.0003v1 [astro-ph.EP].

Notes

  1. ↑ Sum of relative parallax (160.5 ± 3.5 mas) and correction from relative and absolute parallax (3.8 ± 0.5 mas).
  2. ↑ Coincides with Perryman et al. (1997) (Hipparcos) parallax.
  3. ↑ Weighted parallax based on parallaxes from van Altena et al. (1995), Tinney et al. (1995), Tinney (1996), van Leeuwen (2007) and Pravdo & Shaklan (2009).

External links

Coordinates: 19h 16m 58s, +05° 09′ 02″