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)
Details
Mass 0.56 ± 0.08 [6]   M☉
Radius 0.01  R☉
Luminosity 10−3.28 [7]   L☉
Surface gravity (log g)8.27 ± 0.05 [7]   cgs
Temperature 8,490±270 [7]   K
Age (as white dwarf) [7]
1.44  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 an isolated white dwarf located 15.1 light-years (4.6 parsecs ) from the Solar System in the constellation Musca. [16] It is the fourth closest known white dwarf to the Sun, after Sirius B, Procyon B, and van Maanen's star. [17]

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. [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 moving group, which has seven possible members. These stars share a similar motion through space, which may indicate a common origin. [19] This group has an estimated 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 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. [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, [6] but it is the remnant of a massive main-sequence star that had an estimated 4.4 solar masses. [22] 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. [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

Related Research Articles

<span class="mw-page-title-main">Gliese 570</span> Quaternary star system in the constellation Libra

Gliese 570 is a quaternary star system approximately 19 light-years away. The primary star is an orange dwarf star. The other secondary stars are themselves a binary system, two red dwarfs that orbit the primary star. A brown dwarf has been confirmed to be orbiting in the system. In 1998, an extrasolar planet was thought to orbit the primary star, but it was discounted in 2000.

Gliese 65, also known as Luyten 726-8, is a binary star system that is one of Earth's nearest neighbors, at 8.8 light-years from Earth in the constellation Cetus. The two component stars are both flare stars with the variable star designations BL Ceti and UV Ceti.

Gliese 1 is a red dwarf in the constellation Sculptor, which is found in the southern celestial hemisphere. It is one of the closest stars to the Sun, at a distance of 14.2 light years. Because of its proximity to the Earth it is a frequent object of study and much is known about its physical properties and composition. However, with an apparent magnitude of about 8.6 it is too faint to be seen with the naked eye.

Gliese 674(GJ 674) is a small red dwarf star with an exoplanetary companion in the southern constellation of Ara. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.38 and an absolute magnitude of 11.09. The system is located at a distance of 14.85 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −2.9 km/s. It is a candidate member of the 200 million year old Castor stream of co-moving stars.

<span class="mw-page-title-main">Gliese 105</span> Triple star system in the constellation Cetus

Gliese 105 is a triple star system in the constellation of Cetus. It is located relatively near the Sun at a distance of 23.6 light-years. Despite this, even the brightest component is barely visible with the unaided eye (see Bortle scale). No planets have yet been detected around any of the stars in this system.

<span class="mw-page-title-main">Gliese 687</span> Star in the constellation Draco

Gliese 687, or GJ 687 (Gliese–Jahreiß 687) is a red dwarf in the constellation Draco. This is one of the closest stars to the Sun and lies at a distance of 14.84 light-years. Even though it is close by, it has an apparent magnitude of about 9, so it can only be seen through a moderately sized telescope. Gliese 687 has a high proper motion, advancing 1.304 arcseconds per year across the sky. It has a net relative velocity of about 39 km/s. It is known to have a Neptune-mass planet. Old books and articles refer to it as Argelander Oeltzen 17415.

Gliese 673 is an orange dwarf star in the constellation Ophiuchus. It has a stellar classification of K7V. Main sequence stars with this spectra have a mass in the range of 60–70% of solar mass (M☉).

Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°. They are located 15.8 light-years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

<span class="mw-page-title-main">Gliese 445</span> Star in the constellation Camelopardalis

Gliese 445 is an M-type main sequence star in the northern part of the constellation Camelopardalis.

<span class="mw-page-title-main">Gliese 752</span> Binary star system in the constellation Aquila

Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of 19.3 light-years.

Gliese 433 is a dim red dwarf star with multiple exoplanetary companions, located in the equatorial constellation of Hydra. The system is located at a distance of 29.6 light-years from the Sun based on parallax measurements, and it is receding with a radial velocity of +18 km/s. Based on its motion through space, this is an old disk star. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 9.81 and an absolute magnitude of 10.07.

HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

Gliese 179 is a small red dwarf star with an exoplanetary companion in the equatorial constellation of Orion. It is much too faint to be visible to the naked eye with an apparent visual magnitude of 11.94. The system is located at a distance of 40.5 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of –9 km/s. It is a high proper motion star, traversing the celestial sphere at an angular rate of 0.370″·yr−1.

<span class="mw-page-title-main">Stein 2051</span> Star in the constellation Camelopardalis

Stein 2051 is a nearby binary star system, containing a red dwarf and a degenerate star, located in constellation Camelopardalis at about 18 ly from Earth.

Gliese 809 is a red dwarf star in the constellation Cepheus, forming the primary component of a multi-star system. A visual magnitude of 8.55 makes it too faint to see with the naked eye. It is part of the Gliese Catalogue of Nearby Stars and is located about 23 light-years (ly) from the Solar System. Gliese 809 has about 70.5% the radius of the Sun and 61.4% of the Sun's mass. It has a metallicity of −0.06, which means that the abundance of elements other than hydrogen and helium is just 87.1% that of the Sun.

Gliese 180, is a small red dwarf star in the equatorial constellation of Eridanus. It is invisible to the naked eye with an apparent visual magnitude of 10.9. The star is located at a distance of 39 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −14.6 km/s. It has a high proper motion, traversing the sky at the rate of 0.765 arcseconds per year.

GJ 3323 is a nearby single star located in the equatorial constellation Eridanus, about 0.4° to the northwest of the naked eye star Psi Eridani. It is invisible to the naked eye with an apparent visual magnitude 12.20. Parallax measurements give a distance estimate of 17.5 light-years from the Sun. It is drifting further away with a radial velocity of +42.3 km/s. Roughly 104,000 years ago, the star is believed to have come to within 7.34 ± 0.16 light-years of the Solar System.

Gliese 49 is a star in the northern constellation of Cassiopeia. Visually, it is located 106 arcminutes north of the bright star γ Cassiopeiae. With an apparent visual magnitude of 9.56, it is not observable with the naked eye. It is located, based on the reduction of parallax data of Gaia, 32.1 light-years away from the Solar System. The star is drifting closer to the Sun with a radial velocity of −6 km/s.

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 "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 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, doi: 10.1093/mnras/stac3532 , hdl: 10023/26568
  7. 1 2 3 4 Table 2, P. Bergeron; S. K. Leggett; María Teresa Ruiz (April 2001). "Photometric and Spectroscopic Analysis of Cool White Dwarfs with Trigonometric Parallax Measurements". Astrophysical Journal Supplement Series. 133 (2): 413–449. arXiv: astro-ph/0011286 . Bibcode:2001ApJS..133..413B. doi:10.1086/320356. 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. 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. ↑ 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.
  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. ↑ 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.
  20. ↑ Bell, R. A. (1962). "Observations of some southern white dwarfs". The Observatory. 82: 68–71. Bibcode:1962Obs....82...68B.
  21. ↑ 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.
  22. 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.
  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. ↑ 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.
  25. ↑ 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.
  26. ↑ 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.