Astronomy:G 29-38

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Short description: White dwarf which undergoes characteristic variability
G29-38
G29-38 Debris disk.jpg
Artist's impression of G29-38 and its debris disk
Observation data
Equinox J2000.0]] (ICRS)
Constellation Pisces
Right ascension  23h 28m 47.6365s[1]
Declination +05° 14′ 54.235″[1]
Apparent magnitude (V) 13.03[2]
Characteristics
Spectral type DAV4.4[2]
U−B color index −0.63[2]
B−V color index 0.14[2]
V−R color index 0.0[3]
R−I color index 0.2[3]
Variable type DAV (ZZ Ceti)[2]
Astrometry
Radial velocity (Rv)15.3 ± 3.0[3] km/s
Proper motion (μ) RA: −398.246(32)[1] mas/yr
Dec.: −266.744(20)[1] mas/yr
Parallax (π)57.0620 ± 0.0251[1] mas
Distance57.16 ± 0.03 ly
(17.525 ± 0.008 pc)
Details
Mass0.70 ± 0.03[4] M☉
Radius0.01[5] R☉
Luminosity (bolometric)0.002[4] L☉
Surface gravity (log g)8.15 ± 0.05[4] cgs
Temperature11,820 ± 175[4] K
Other designations
ZZ Piscium, EGGR 159, GJ 895.2, LHS 5405, LTT 16907, NLTT 56992, WD 2326+049.[3]
Database references
SIMBADdata

Giclas 29-38, also known as ZZ Piscium, is a variable white dwarf star of the DAV (or ZZ Ceti) type, whose variability is due to large-amplitude, non-radial pulsations known as gravity waves. It was first reported to be variable by Shulov and Kopatskaya in 1974.[6][7] DAV stars are like normal white dwarfs but have luminosity variations with amplitudes as high as 30%, arising from a superposition of vibrational modes with periods from 100 to 1,000 seconds. Large-amplitude DAVs generally differ from lower-amplitude DAVs by having lower temperatures, longer primary periodicities, and many peaks in their vibrational spectra with frequencies which are sums of other vibrational modes.[8]

A light curve for ZZ Piscium, adapted from Fontaine and Brassard (2008)[9]

G29-38, like other complex, large-amplitude DAV variables, has proven difficult to understand. The power spectrum or periodogram of the light curve varies over times which range from weeks to years. Usually, one strong mode dominates, although many smaller-amplitude modes are often observed. The larger-amplitude modes, however, fluctuate in and out of observability; some low-power areas show more stability. Asteroseismology uses the observed spectrum of pulsations from stars like G29-38 to infer the structure of their interiors.[8]

The spectrum of G29-38

Debris disk

The circumstellar environment of G29-38 first attracted attention in the late 1980s during a near-infrared survey of 200 white dwarfs conducted by Ben Zuckerman and Eric Becklin to search for low mass companion stars and brown dwarfs.[10] G29-38 was shown to radiate substantial emission between 2 and 5 micrometres, far in excess of that expected from extrapolation of the visual and near infrared spectrum of the star.[11] Like other young, hot white dwarfs, G29-38 is thought to have formed relatively recently (600 million years ago) from its AGB progenitor, and therefore the excess was naturally explained by emission from a Jupiter-like brown dwarf with a temperature of 1200 K and a radius of 0.15 solar radius.[10][11] However, later observations, including speckle interferometry, failed to detect a brown dwarf.[12]

Infrared observations made in 2004 by NASA's Spitzer Space Telescope indicated the presence of a dust cloud around G29-38, which may have been created by tidal disruption of an exocomet or exoasteroid passing close to the white dwarf.[13] This may mean that G29-38 is still orbited by a ring of surviving comets and, possibly, outer planets. This is the first observation supporting the idea that comets persist to the white dwarf stage of stellar evolution.[14]

Infrared emission at 9-11 Mircons from Spitzer spectroscopy were interpreted as a mixture of amorphous olivine and a small amount of fosterite in the disk.[13] Modelling of the disk have shown that the inner edge of the disk lies at around 96±4 white dwarf radii and that the disk has a width of about 1-10 white dwarf radii. The dust mass of the disk is about 4-5 x 1018 g (about half the mass of a massive asteroid) and the disk has a temperature less than 1000 K.[15]

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 The general catalogue of trigonometric parallaxes, W. F. van Altena, J. T. Lee, E. D. Hoffleit, New Haven, CT: Yale University Observatory, c1995, 4th ed., completely revised and enlarged. CDS ID I/238A.
  3. ↑ 3.0 3.1 3.2 3.3 "V* ZZ Psc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+ZZ+Psc. 
  4. ↑ 4.0 4.1 4.2 4.3 Table 1, The Formation Rate and Mass and Luminosity Functions of DA White Dwarfs from the Palomar Green Survey, James Liebert, P. Bergeron, and J. B. Holberg, The Astrophysical Journal Supplement Series 156, #1 (January 2005), pp. 47–68, doi:10.1086/425738, Bibcode: 2005ApJS..156...47L.
  5. ↑ §1, The Dust cloud around the White Dwarf G 29-38. 2. Spectrum from 5-40 microns and mid-infrared variability, William T. Reach, Carey Lisse, Ted von Hippel, and Fergal Mullally, Astrophysical Journal, in press, Bibcode: 2008arXiv0810.3276R.
  6. ↑ O. S. Shulov and E. N. Kopatskaya, Astrofizika 10, #1 (January–March, 1974), pp. 117–120. Translated into English as Variability of the white dwarf G 29-38, Astrophysics, 10, #1 (January, 1974), pp. 72–74. DOI 10.1007/BF01005183.
  7. ↑ G 29-38 and G 38-29: two new large-amplitude variable white dwarfs, J. T. McGraw and E. L. Robinson, Astrophysical Journal 200 (September 1975), pp. L89–L93.
  8. ↑ 8.0 8.1 Observational limits on companions to G29-38, S. J. Kleinman, R. E. Nather, D. E. Winget, J. C. Clemens, P. A. Bradley, A. Kanaan, J. L. Provencal, C. F. Claver, T. K. Watson, K. Yanagida, J. S. Dixson, M. A. Wood, D. J. Sullivan, E. Meistas, E. M. Leibowitz, P. Moskalik, S. Zola, G. Pajdosz, J. Krzesinski, J.-E. Solheim, A. Bruvold, D. O'Donoghue, M. Katz, G. Vauclair, N. Dolez, M. Chevreton, M. A. Barstow, S. O. Kepler, O. Giovannini, C. J. Hansen, and S. D. Kawaler, Astrophysical Journal 436, #2 (December 1994), pp. 875–884.
  9. ↑ Fontaine, G.; Brassard, P. (October 2008). "The Pulsating White Dwarf Stars". Publications of the Astronomical Society of the Pacific 120 (872): 1043. doi:10.1086/592788. Bibcode: 2008PASP..120.1043F. 
  10. ↑ 10.0 10.1 A low-temperature companion to a white dwarf star, E. E. Becklin & B. Zuckerman, Nature 336 (Dec. 15, 1988), pp. 656-658
  11. ↑ 11.0 11.1 Excess infrared radiation from a white dwarf - an orbiting brown dwarf? B. Zuckerman & E. E. Becklin, Nature 330, (Nov. 12, 1987), pp. 138-140
  12. ↑ Keck Speckle Imaging of the White Dwarf G29-38: No Brown Dwarf Companion Detected, Marc J. Kuchner, Christopher D. Koresko, and Michael E. Brown, The Astrophysical Journal 508, #1 (November 20, 1998), pp. L81–L83. doi:10.1086/311725. Bibcode: 1998ApJ...508L..81K.
  13. ↑ 13.0 13.1 The Dust Cloud around the White Dwarf G29-38, William T. Reach, Marc J. Kuchner, Ted von Hippel, Adam Burrows, Fergal Mullally, Mukremin Kilic, and D. E. Winget, Astrophysical Journal 635, #2 (December 2005), pp. L161–L164.
  14. ↑ NASA's Spitzer Finds Possible Comet Dust Around Dead Star , NASA press release, January 11, 2006.
  15. ↑ Ballering, Nicholas P.; Levens, Colette I.; Su, Kate Y. L.; Cleeves, L. Ilsedore (2022-11-01). "The Geometry of the G29-38 White Dwarf Dust Disk from Radiative Transfer Modeling". The Astrophysical Journal 939 (2): 108. doi:10.3847/1538-4357/ac9a4a. ISSN 0004-637X. Bibcode: 2022ApJ...939..108B. 

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