Gliese 440

Last updated
Gliese 440
LAWD 37 (heic2301a).jpg
Gliese 440 seen by the Hubble Space Telescope [1]
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Musca [2]
Right ascension 11h 45m 42.91694s [3]
Declination −64° 50′ 29.4620″ [3]
Apparent magnitude  (V)11.50 [4]
Characteristics
Spectral type DQ6 [5]
U−B color index -0.59 [4]
B−V color index +0.19 [4]
Astrometry
Proper motion (μ)RA: 2661.640 mas/yr [3]
Dec.: -344.933 mas/yr [3]
Parallax (π)215.6753±0.0181  mas [3]
Distance 15.123 ± 0.001  ly
(4.6366 ± 0.0004  pc)
Absolute magnitude  (MV)+13.17±0.03 [6]
Details
Mass 0.56±0.08 [7]   M☉
Radius 0.0127±0.0003 [7]   R☉
Luminosity 5.25+0.64
−0.57×10−4 [6]   L☉
Surface gravity (log g)7.983±0.016 [7]   cgs
Temperature 7,837+87
−82 [7]   K
Age (as white dwarf) 1.21±0.09 [6]   Gyr
Other designations
GJ 440 [8] , HIP 57367 [9] , BPM 7108, Ci 20 658 [10] , EG GR 82, L 145-141, LAWD 37, LHS 43 [11] , LP 145-141, LPM 396, LTT 4364, NLTT 28447 [12] , PLX 2716 [13] , PM 11429-6434, WD 1142-645, TYC 8981-4417-1 [14] [15] , GSC 08981-04418, 2MASS J11454297-6450297
Database references
SIMBAD data
Musca constellation map.svg
Red pog.png
Gliese 440
Location of Gliese 440 in the constellation Musca

Gliese 440, also known as LP 145-141 or LAWD 37, [4] is a white dwarf located 15.1 light-years (4.6 parsecs ) from the Solar System in the constellation Musca, the nearest star in this constellation. [16] [17] It is the fourth closest white dwarf, after Sirius B, Procyon B, and van Maanen's star. [18] Despite its closeness, Gliese 440 is intrinsically faint with just 0.05% the luminosity of the Sun, and can not be viewed to the naked eye with an apparent magnitude of +11.5. [4] [6]

Contents

History of observations

Gliese 440 is known at least from 1917, when its proper motion was published by R. T. A. Innes and H. E. Wood in Volume 37 of Circular of the Union Observatory. [19] The corresponding designation is UO 37. [10] (Note: this designation is not unique for this star, that is all other stars, listed in the table in the Volume 37 of this Circular, also could be called by this name).

Space motion

Gliese 440 may be a member of the Wolf 219 moving group, which has seven possible members. These stars share a similar motion through space, which may indicate a common origin. [20] This group has an estimated space velocity of 160 km/s and is following a highly eccentric orbit through the Milky Way galaxy. [21]

Properties

White dwarfs are no longer generating energy at their cores through nuclear fusion, and instead are steadily radiating away their remaining heat. Gliese 440 has a DQ spectral classification, indicating that it is a rare type of white dwarf which displays evidence of atomic or molecular carbon in its spectrum. [22]

Gliese 440 is small and faint, like typical white dwarfs, having just 0.0127 times the Sun's radius (1.4 times Earth's radius) and 0.05 percent the Sun's luminosity. Gliese 440 currently has an effective temperature of 7,800  K and will cool as its residual heat escape to the cosmos. The rate of cooling allows its age in the white dwarf stage to be estimated at 1.2 billion years. [6] [7]

In 2019, Gliese 440 was observed passing in front of a more distant star. The bending of starlight by the gravitational field of Gliese 440 was observed by the Hubble Space Telescope, allowing its mass to be directly measured at 0.56±0.08  M☉ . The mass fits the expected range of a white dwarf with a carbon-oxygen core. This was the second mass determination of a white dwarf using this method, after Stein 2051 B. [7]

Gliese 440 is the remnant of a massive B-type star that had an estimated 4.4 solar masses. [23] [24] While it was on the main sequence, it probably was a spectral class B star (in the range B4–B9). [23] Most of the star's original mass was shed after it passed into the asymptotic giant branch stage, just prior to becoming a white dwarf.

Search for companions

A survey with the Hubble Space Telescope revealed no visible orbiting companions, at least down to the limit of detection. [25] [5]

Its proximity, mass and temperature have led to it being considered a good candidate to look for Jupiter-like planets. Its relatively large mass and high temperature mean that the system is relatively short-lived and hence of more recent origin. [24]

Hipparcos-Gaia proper motion shows an anomaly that hints to the presence of an exoplanet that has a mass of either 0.44 or 0.60 MJ which is between Saturn and Jupiter. [26] [27]

See also

References

  1. ↑ "LAWD 37". esahubble.org. 2 February 2023. Archived from the original on 22 April 2023. Retrieved 21 April 2023.
  2. ↑ "Constellation boundaries". Centre de Données astronomiques de Strasbourg. Archived from the original on 2019-07-17. Retrieved 2007-07-16.
  3. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  4. 1 2 3 4 5 "LAWD 37". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2007-07-16.
  5. 1 2 Daniel J. Schroeder; et al. (February 2000). "A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2". The Astronomical Journal. 119 (2): 906–922. Bibcode:2000AJ....119..906S. doi: 10.1086/301227 .
  6. 1 2 3 4 5 Subasavage, John P.; et al. (July 2017). "The Solar Neighborhood. XXXIX. Parallax Results from the CTIOPI and NOFS Programs: 50 New Members of the 25 parsec White Dwarf Sample". The Astronomical Journal. 154 (1): 24. arXiv: 1706.00709 . Bibcode:2017AJ....154...32S. doi: 10.3847/1538-3881/aa76e0 . S2CID   119189852. 32.{{cite journal}}: CS1 maint: postscript (link)
  7. 1 2 3 4 5 6 McGill, P.; Anderson, J.; Casertano, S.; Sahu, K.C. (March 2023). "First semi-empirical test of the white dwarf mass-radius relationship using a single white dwarf via astrometric microlensing". Monthly Notices of the Royal Astronomical Society. 520 (1): 259–280. arXiv: 2206.01814 . doi: 10.1093/mnras/stac3532 . hdl: 10023/26568 .
  8. ↑ Gliese, W.; Jahreiß, H. (1991). "Gl 440". Preliminary Version of the Third Catalogue of Nearby Stars. Archived from the original on 2016-03-04. Retrieved 2015-09-21.
  9. ↑ Perryman; et al. (1997). "HIP 57367". The Hipparcos and Tycho Catalogues. Archived from the original on 2016-03-04. Retrieved 2015-09-21.
  10. 1 2 Porter, J. G.; Yowell, E. J.; Smith, E. S. (1930). "A catalogue of 1474 stars with proper motion exceeding four-tenths year". Publications of the Cincinnati Observatory. 20: 1–32. Bibcode:1930PCinO..20....1P. Page 16 (Ci 20 658). Archived 2023-03-20 at the Wayback Machine
  11. ↑ Luyten, Willem Jacob (1979). "LHS 30". LHS Catalogue, 2nd Edition. Archived from the original on 2016-03-04. Retrieved 2015-10-15.
  12. ↑ Luyten, Willem Jacob (1979). "NLTT 28447". NLTT Catalogue. Archived from the original on 2016-03-04. Retrieved 2015-10-15.
  13. ↑ Van Altena W. F.; Lee J. T.; Hoffleit E. D. (1995). "GCTP 2716". The General Catalogue of Trigonometric Stellar Parallaxes (Fourth ed.). Archived from the original on 2016-03-04. Retrieved 2015-09-21.
  14. ↑ Perryman; et al. (1997). "HIP 57367". The Hipparcos and Tycho Catalogues. Archived from the original on 2016-03-04. Retrieved 2015-09-21.
  15. ↑ Hog; et al. (2000). "TYC 8981-4417-1". The Tycho-2 Catalogue. Archived from the original on 2016-03-04. Retrieved 2015-10-15.
  16. ↑ Henry, Todd J.; Walkowicz, Lucianne M.; Barto, Todd C.; Golimowski, David A. (April 2002). "The Solar Neighborhood. VI. New Southern Nearby Stars Identified by Optical Spectroscopy". The Astronomical Journal. 123 (4): 2002–2009. arXiv: astro-ph/0112496 . Bibcode:2002AJ....123.2002H. doi:10.1086/339315. S2CID   17735847.
  17. ↑ Kirkpatrick, J. Davy; Marocco, Federico; et al. (April 2024). "The Initial Mass Function Based on the Full-sky 20 pc Census of ~3600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series . 271 (2): 55. arXiv: 2312.03639 . Bibcode:2024ApJS..271...55K. doi: 10.3847/1538-4365/ad24e2 .
  18. ↑ Table 1, Sion Edward M (2009). "The white dwarfs within 20 parsecs of the sun: kinematics and statistics". The Astronomical Journal. 138 (6): 1681–1689. arXiv: 0910.1288 . Bibcode:2009AJ....138.1681S. doi:10.1088/0004-6256/138/6/1681. S2CID   119284418.
  19. ↑ Innes & Wood (1917). Archived 2016-01-20 at the Wayback Machine Page 290 (see string 41). Archived 2015-01-28 at the Wayback Machine
  20. ↑ Eggen, O. J.; Greenstein, J. L. (1965). "Spectra, colors, luminosities, and motions of the white dwarfs". Astrophysical Journal. 141: 83–108. Bibcode:1965ApJ...141...83E. doi:10.1086/148091.— see table 5.
  21. ↑ Bell, R. A. (1962). "Observations of some southern white dwarfs". The Observatory. 82: 68–71. Bibcode:1962Obs....82...68B.
  22. ↑ Kawaler, S.; Dahlstrom, M. (2000). "White Dwarf Stars". American Scientist. 88 (6): 498. Bibcode:2000AmSci..88..498K. doi:10.1511/2000.6.498. S2CID   227226657. Archived from the original on April 18, 2005. Retrieved 2007-07-19.
  23. 1 2 Siess, Lionel (2000). "Computation of Isochrones". Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles. Archived from the original on 2011-05-05. Retrieved 2007-03-24.
  24. 1 2 Burleigh, M. R.; Clarke, F. J.; Hodgkin, S. T. (April 2002). "Imaging planets around nearby white dwarfs". Monthly Notices of the Royal Astronomical Society. 331 (4): L41 –L45. arXiv: astro-ph/0202194 . Bibcode:2002MNRAS.331L..41B. doi: 10.1046/j.1365-8711.2002.05417.x . S2CID   18383063.
  25. ↑ Jao, Wei-Chun; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer L.; Costa, Edgardo; Méndez, René A. (2005). "The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with mu >= 1.0" yr-1 (MOTION Sample)". The Astronomical Journal . 129 (4): 1954–1967. arXiv: astro-ph/0502167 . Bibcode:2005AJ....129.1954J. doi:10.1086/428489. S2CID   16164903.
  26. ↑ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022-01-01). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs". Astronomy and Astrophysics. 657: A7. arXiv: 2109.10912 . Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. ISSN   0004-6361. Archived from the original on 2023-12-17. Retrieved 2023-05-15.
  27. ↑ Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019-03-01). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy and Astrophysics. 623: A72. arXiv: 1811.08902 . Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. ISSN   0004-6361. Archived from the original on 2023-06-10. Retrieved 2023-05-15.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.