LP 145-141

LP 145-141
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Musca[1]
Right ascension 11h 45m 42.9205s[2]
Declination −64° 50′ 29.459″[2]
Apparent magnitude (V) 11.50[2]
Characteristics
Spectral type DQ6[3]
U−B color index -0.59[2]
B−V color index +0.19[2]
Astrometry
Proper motion (μ) RA: 2665.25[2] mas/yr
Dec.: -346.19[2] mas/yr
Parallax (π)215.80 ± 1.25[4] mas
Distance15.11 ± 0.09 ly
(4.63 ± 0.03 pc)
Details
Mass0.75 ± 0.03[5] M☉
Luminosity0.0005[5] L☉
Surface gravity (log g)8.27 ± 0.05[5] cgs
Temperature8,500 ± 300[5] K
Age(as white dwarf)[5]
1.44·109 years
Other designations
UO 37[6]
Ci 20 658[7]
LPM 396
L 145-141
LTT 4364
LAWD 37
BPM 7108
LP 145-141
EGGR 82
WD 1142-645
PM 11429-6434
NLTT 28447[8]
LHS 43[9]
GJ 440[10]
PLX 2716[11]
GSC 08981-04418
HIP 57367[12]
TYC 8981-4417-1[13][14]
2MASS J11454297-6450297
Database references
SIMBADdata

LP 145-141 is a white dwarf located 15 light years from the Solar System.[15] According to a 2009 paper, it is the fourth closest known white dwarf to the Sun (after Sirius B, Procyon B, and van Maanen's star.)[16]

History of observations

LP 145-141 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.[6] The corresponding designaion is UO 37.[7] (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).

Distance

LP 145-141 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Woolley et al. (1970) 206±8 4.85+0.2
−0.18		 15.8±0.6 149.8+6.1
−5.6		 [17]
Gliese & Jahreiß (1991) 218.5±5.0 4.58+0.11
−0.1		 14.9±0.3 141.2+3.3
−3.2		 [10]
van Altena et al. (1995) 218.3±6.7 4.58+0.15
−0.14		 14.9+0.5
−0.4		 141.4+4.5
−4.2		 [11]
Perryman et al. (1997) (Hipparcos) 216.40±2.11 4.62+0.05
−0.04		 15.07±0.15 142.6±1.4 [12]
Perryman et al. (1997) (Tycho) 244.20±71.00 4.1+1.7
−0.9		 13.4+5.5
−3		 126.4+51.8
−28.5		 [13]
Jao et al. (2005) 215.07±2.04 4.65±0.04 15.17+0.15
−0.14		 143.5+1.4
−1.3		 [18]
van Leeuwen (2007) 217.01±2.40 4.61±0.05 15.03+0.17
−0.16		 142.2±1.6 [19]
Subasavage et al. (2009) 215.80±1.25 4.634±0.027 15.11±0.09 143±0.8 [4]
RECONS TOP100 (2012) 216.12±1.09[nb 1] 4.627±0.023 15.09±0.08 142.8±0.7 [20]

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

Space motion

LP 145-141 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.[21] This group has an estimated space velocity of 160 km/s and is following a highly eccentric orbit through the Milky Way galaxy.[22]

LP 145-141 proper motion estimates

Source μ, mas/yr P. A., ° μRA, mas/yr μDEC, mas/yr Ref.
Innes & Wood (1917)2690992656.9−420.8[6]
Hog et al. (2000)2692 ± 497.53 ± 0.092668.5 ± 4.0−352.7 ± 3.8[14]
van Leeuwen (2007)2686.5 ± 2.597.43 ± 0.052663.91 ± 2.21−347.38 ± 2.07[19]

The most accurate estimates are marked in bold. Italic are computed values, not italic are values, given in the sources.

Properties

White dwarfs are no longer generating energy at their cores through nuclear fusion, and instead are steadily radiating away their remaining heat. LP 145-141 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.[23]

LP 145-141 has only 75% of the Sun's mass, but it is the remnant of a massive main-sequence star that had an estimated 4.4 solar masses.[24] While it was on the main sequence, it probably was a spectral class B star (in the range B4-B9).[25] 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.[3]

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.[26]

References

  1. ↑ "Constellation boundaries". Centre de Données astronomiques de Strasbourg. Retrieved 2007-07-16.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 "SIMBAD query result: GJ 440 -- White Dwarf". Centre de Données astronomiques de Strasbourg. Retrieved 2007-07-16.
  3. ↑ 3.0 3.1 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.
  4. ↑ 4.0 4.1 Subasavage, J. P.; Jao, W. C.; Henry, T. J.; Bergeron, P.; Dufour, P.; Ianna, P. A.; Costa, E.; Méndez, R. A. (2009). "The Solar Neighborhood. XXI. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the 25 Parsec White Dwarf Sample". The Astronomical Journal 137 (6): 4547–4560. arXiv:0902.0627. Bibcode:2009AJ....137.4547S. doi:10.1088/0004-6256/137/6/4547.
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Table 2, P. Bergeron, S. K. Leggett, and 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.
  6. ↑ 6.0 6.1 6.2 Innes & Wood (1917). Page 290 (see string 41).
  7. ↑ 7.0 7.1 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).
  8. ↑ Luyten, Willem Jacob (1979). "NLTT 28447". NLTT Catalogue.
  9. ↑ Luyten, Willem Jacob (1979). "LHS 30". LHS Catalogue, 2nd Edition.
  10. ↑ 10.0 10.1 Gliese, W. and Jahreiß, H. (1991). "Gl 440". Preliminary Version of the Third Catalogue of Nearby Stars.
  11. ↑ 11.0 11.1 Van Altena W. F., Lee J. T., Hoffleit E. D. (1995). "GCTP 2716". The General Catalogue of Trigonometric Stellar Parallaxes (Fourth ed.).
  12. ↑ 12.0 12.1 Perryman et al. (1997). "HIP 57367". The Hipparcos and Tycho Catalogues.
  13. ↑ 13.0 13.1 Perryman et al. (1997). "HIP 57367". The Hipparcos and Tycho Catalogues.
  14. ↑ 14.0 14.1 Hog et al. (2000). "TYC 8981-4417-1". The Tycho-2 Catalogue.
  15. ↑ 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.
  16. ↑ Table 1, "The White Dwarfs Within 20 Parsecs of the Sun: Kinematics and Statistics", Edward M. Sion et al., The Astronomical Journal 138, #6 (December 2009), pp. 1681-1689, doi:10.1088/0004-6256/138/6/1681, Bibcode: 2009AJ....138.1681S.
  17. ↑ Woolley R.; Epps E. A.; Penston M. J.; Pocock S. B. (1970). "Woolley 440". Catalogue of stars within 25 parsecs of the Sun.
  18. ↑ 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.
  19. ↑ 19.0 19.1 van Leeuwen F. (2007). "HIP 57367". Validation of the new Hipparcos reduction.
  20. ↑ "RECONS TOP100". THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars). 2012.
  21. ↑ 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.
  22. ↑ Bell, R. A. (1962). "Observations of some southern white dwarfs". The Observatory 82: 68–71. Bibcode:1962Obs....82...68B.
  23. ↑ Kawaler, S.; Dahlstrom, M. (2000). "White Dwarf Stars". American Scientist 88 (6): 498. Bibcode:2000AmSci..88..498K. doi:10.1511/2000.6.498. Retrieved 2007-07-19.
  24. ↑ 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.
  25. ↑ Siess, Lionel (2000). "Computation of Isochrones". Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles. Retrieved 2007-03-24.
  26. ↑ Burleigh, Matthew R.; Clarke, F.J.; Hodgkin, S.T. (2002). "Imaging Planets around Nearby White Dwarfs" (PDF). 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.

Notes

  1. ↑ Weighted parallax based on parallaxes from van Altena et al. (1995), van Leeuwen (2007), Jao et al. (2005) and Subasavage et al. (2009).

External links