Ross 548

In this article, we will explore the fascinating world of Ross 548 and its implications on modern society. From its origins to its impact today, Ross 548 has been the subject of debate, discussion and constant interest. Over the years, Ross 548 has proven its relevance in various fields, from politics to science to popular culture. Through this comprehensive analysis, we will seek to better understand the importance of Ross 548 in today's world and how it has shaped the way we think, act, and relate to the environment around us. Join us on this journey of discovery and reflection about Ross 548.

Ross 548

A light curve for ZZ Ceti, adapted from Stover et al. (1980)[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cetus
Right ascension 01h 36m 13.61558s[2]
Declination −11° 20′ 32.6318″[2]
Apparent magnitude (V) 14.16±0.01[3]
Characteristics
Evolutionary stage White dwarf
Spectral type DA4.0[4]
U−B color index −0.5[5]
B−V color index 0.2[5]
Variable type ZZ Cet (DAV)[5]
Astrometry
Proper motion (μ) RA: +460.845[2] mas/yr
Dec.: −116.448[2] mas/yr
Parallax (π)30.5249±0.0546 mas[2]
Distance106.8 ± 0.2 ly
(32.76 ± 0.06 pc)
Absolute magnitude (MV)11.78±0.06[6]
Details[6]
Mass0.65±0.02 M☉
Radius0.0118±0.0002 R☉
Luminosity0.0029±0.0002 L☉
Surface gravity (log g)8.108±0.025 cgs
Temperature12,281±125 K
Rotation37.84±1.99 h
Other designations
ZZ Cet, EGGR 10, G 271-106, G 272-52, LTT 873, NLTT 5358, WD 0133-116[7]
Database references
SIMBADdata

Ross 548 is a white dwarf in the equatorial constellation of Cetus.[7] With a mean apparent visual magnitude of 14.2[3] it is much too faint to be visible to the naked eye. Based on parallax measurements, it is located at a distance of 107 light years from the Sun.[2] It was found to be variable in 1970[8] and in 1972 it was given the variable star designation ZZ Ceti.[9] This is a pulsating white dwarf of the DAV type that is the prototype of the ZZ Ceti variable class.[10], pp. 891, 895.[3]

This DA-class white dwarf is the surviving core of a red giant star that ceased nuclear fusion while shedding its outer envelope. It has a (presumably) homogeneous core of carbon and oxygen, a relatively thin outer envelope of hydrogen, and a helium mantle. The object has 65% of the mass of the Sun, with 1.2% of the Sun's radius. It is radiating 0.3% of the luminosity of the Sun at an effective temperature of 12,281 K. Ross 548 is spinning with a period of ~38 hours.[6] The dominant pulsation mode of this object has a period of 213.1326 seconds. It has up to 11 known pulsation modes in total.[3]

References

  1. ^ Stover, R. J.; Hesser, James E.; Lasker, Barry M.; Nather, R. E.; Robinson, E. L. (September 1980). "Period stability of the pulsating white dwarf R 548 (=ZZ Ceti)". The Astrophysical Journal. 240: 865–870. Bibcode:1980ApJ...240..865S. doi:10.1086/158300.
  2. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. ^ a b c d Giammichele, N.; et al. (December 2015). "A New Analysis of the Two Classical ZZ Ceti White Dwarfs GD 165 and Ross 548. I. Photometry and Spectroscopy". The Astrophysical Journal. 815 (1): 12. Bibcode:2015ApJ...815...56G. doi:10.1088/0004-637X/815/1/56. S2CID 125328132. 56.
  4. ^ Gianninas, A.; et al. (December 2011). "A Spectroscopic Survey and Analysis of Bright, Hydrogen-rich White Dwarfs". The Astrophysical Journal. 743 (2): 27. arXiv:1109.3171. Bibcode:2011ApJ...743..138G. doi:10.1088/0004-637X/743/2/138. S2CID 119210906. 138.
  5. ^ a b c McCook, George P.; Sion, Edward M. (March 1999). "A Catalog of Spectroscopically Identified White Dwarfs". Astrophysical Journal Supplement. 121 (1): 1–130. Bibcode:1999ApJS..121....1M. doi:10.1086/313186. S2CID 122286998. CDS ID III/210.
  6. ^ a b c Giammichele, N.; et al. (March 2016). "A New Analysis of the Two Classical ZZ Ceti White Dwarfs GD 165 and Ross 548. II. Seismic Modeling". The Astrophysical Journal Supplement Series. 223 (1): 27. Bibcode:2016ApJS..223...10G. doi:10.3847/0067-0049/223/1/10. S2CID 124354534. 10.
  7. ^ a b "ZZ Cet". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-16.{{cite web}}: CS1 maint: postscript (link)
  8. ^ Lasker, Barry M.; Hesser, James E. (February 1971). "High-Frequency Stellar Oscillations. VI. R548, a Periodically Variable White Dwarf". Astrophysical Journal. 163: L89 – L93. Bibcode:1971ApJ...163L..89L. doi:10.1086/180673.
  9. ^ Kukarkin, B. V.; et al. (September 21, 1972). "58th Name-List of Variable Stars". Information Bulletin on Variable Stars. 717: 1. Bibcode:1972IBVS..717....1K.
  10. ^ Koester, D.; Chanmugam, G. (1990). "Physics of white dwarf stars". Reports on Progress in Physics. 53 (7): 837–915. Bibcode:1990RPPh...53..837K. doi:10.1088/0034-4885/53/7/001. S2CID 250915046.