Gliese 440

Coordinates: Sky map 11h 45m 42.9205s, −64° 50′ 29.459″
Source: Wikipedia, the free encyclopedia.
Gliese 440

Gliese 440 seen by the Hubble Space Telescope[1]
Observation data
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]
Distance
15.123 ± 0.001 ly
(4.6366 ± 0.0004 pc)
Details
Gyr
TYC 8981-4417-1[14][15], GSC 08981-04418, 2MASS
J11454297-6450297
Database references
SIMBADdata
Gliese 440 is located in the constellation Musca.
Gliese 440 is located in the constellation Musca.
Gliese 440
Location of Gliese 440 in the constellation Musca

Gliese 440, also known as LP 145-141 or LAWD 37,

van Maanen's star.[17]

History of observations

Gliese 440 is known at least from 1917, when its

R. T. A. Innes and H. E. Wood in Volume 37 of Circular of the Union Observatory.[18] 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

space velocity of 160 km/s and is following a highly eccentric orbit through the Milky Way galaxy.[20]

Properties

White dwarfs are no longer generating energy at their cores through

spectral classification, indicating that it is a rare type of white dwarf which displays evidence of atomic or molecular carbon in its spectrum.[21]

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 observed by the Hubble Space Telescope allowed its mass to be directly measured. The estimated mass of Gliese 440 is 0.56±0.08 M☉, which fits the expected range of a white dwarf with a carbon-oxygen core. This measurement marked the first direct gravitational mass determination of a single white dwarf.[6]

Gliese 440 has only 56% of the Sun's mass,

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.[24][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.[22]

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.[25][26]

See also

  • List of nearest stars and brown dwarfs

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. ^
    S2CID 244398875
    . Gaia DR3 record for this source at VizieR.
  4. ^ a b c d "LAWD 37". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2007-07-16.
  5. ^
    doi:10.1086/301227
    .
  6. ^
    hdl:10023/26568
    , retrieved 2023-02-08
  7. ^
    S2CID 15511301
    .
  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. ^
    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. S2CID 17735847
    .
  17. S2CID 119284418
    .
  18. ^ Innes & Wood (1917). Archived 2016-01-20 at the Wayback Machine Page 290 (see string 41). Archived 2015-01-28 at the Wayback Machine
  19. doi:10.1086/148091
    . — see table 5.
  20. Bibcode:1962Obs....82...68B
    .
  21. S2CID 227226657. Archived from the original
    on April 18, 2005. Retrieved 2007-07-19.
  22. ^
    S2CID 18383063
    .
  23. ^ 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. S2CID 16164903
    .
  25. ISSN 0004-6361. Archived
    from the original on 2023-12-17. Retrieved 2023-05-15.
  26. ISSN 0004-6361. Archived
    from the original on 2023-06-10. Retrieved 2023-05-15.

External links
Retrieved from "https://en.wikipedia.org/w/index.php?title=Gliese_440&oldid=1230483341"