GD 358

{{Short description|Star in the constellation Hercules}}

{{redirect|V777 Herculis|the star type|Pulsating white dwarf}}

{{Starbox begin |

name=[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=GD%20358 GD 358] }}

{{Starbox image

| image = 250px

| caption = A white-light light curve for GD 358, adapted from Winget et al. (1982)

}}

{{Starbox observe |

epoch=J2000.0 (ICRS) |

constell=Hercules |

ra={{RA|16|47|19.02}}{{cite simbad|title=GD 358|access-date=June 12, 2007}} |

dec={{DEC|+32|28|31.9}} |

appmag_v=13.65}}

{{Starbox character |

b-v=-0.1 |

class=DBV2[http://adsabs.harvard.edu/abs/1999ApJS..121....1M A Catalog of Spectroscopically Identified White Dwarfs], George P. McCook and Edward M. Sion, Astrophysical Journal Supplement 121, #1 (March 1999), pp. 1–130. CDS ID [http://vizier.u-strasbg.fr/viz-bin/Cat?III/210 III/210]. |

variable=DBV }}

{{Starbox astrometry |

prop_mo_ra=6 |

prop_mo_dec=-162 |

parallax = 23.2012 |

p_error = 0.0298 |

parallax_footnote = {{cite DR2|1314045729544380288}} |

absmag_v = +10.33{{cite journal|bibcode=2015ApJS..219...19L|title=Physical Properties of the Current Census of Northern White Dwarfs within 40 pc of the Sun|journal=The Astrophysical Journal Supplement Series|volume=219|issue=2|pages=19|last1=Limoges|first1=M. -M|last2=Bergeron|first2=P.|last3=Lépine|first3=S.|year=2015|doi=10.1088/0067-0049/219/2/19|arxiv=1505.02297|s2cid=118494290}}

}}

{{starbox detail

| source = {{cite journal|doi=10.1051/0004-6361/202142153|title=Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS. III. Asteroseismology of the DBV star GD 358|year=2022|last1=Córsico|first1=A. H.|last2=Uzundag|first2=M.|last3=Kepler|first3=S. O.|last4=Silvotti|first4=R.|last5=Althaus|first5=L. G.|last6=Koester|first6=D.|last7=Baran|first7=A. S.|last8=Bell|first8=K. J.|last9=Bischoff-Kim|first9=A.|last10=Hermes|first10=J. J.|last11=Kawaler|first11=S. D.|last12=Provencal|first12=J. L.|last13=Winget|first13=D. E.|last14=Montgomery|first14=M. H.|last15=Bradley|first15=P. A.|last16=Kleinman|first16=S. J.|last17=Nitta|first17=A.|journal=Astronomy & Astrophysics|volume=659|pages=A30|arxiv=2111.15551|s2cid=244729212|bibcode=2022A&A...659A..30C}}

| mass = {{val|0.584|0.025|0.019}}

| temperature = {{val|24967|200|fmt=commas}}

| radius = {{val|0.0132|0.0004}}

| radius_km = {{val|{{cvt|0.0131825673856|solar radius|km|sigfig=3|disp=number}}|{{cvt|0.0004318794391|solar radius|km|sigfig=2|disp=number}}|{{cvt|0.0004181792975|solar radius|km|sigfig=2|disp=number}}|fmt=commas}}

| luminosity = {{val|0.061|0.002}}

| gravity = {{val|7.964|0.048|0.043}}

| age_gyr =

}}

{{Starbox catalog |

names=EGGR 239, V777 Her, PG 1645+325, WD 1645+325. }}

{{Starbox reference

| Simbad = GD+358

}}

{{Starbox end}}

GD 358 is a variable white dwarf star of the DBV type. Like other pulsating white dwarfs, its variability arises from non-radial gravity wave pulsations within the star itself.{{Cite journal |last=Winget |first=D E |date=1998-12-14 |title=Asteroseismology of white dwarf stars |url=https://dx.doi.org/10.1088/0953-8984/10/49/014 |journal=Journal of Physics: Condensed Matter |volume=10 |issue=49 |pages=11247–11261 |doi=10.1088/0953-8984/10/49/014 |bibcode=1998JPCM...1011247W |s2cid=250749380 |issn=0953-8984|url-access=subscription }} GD 358 was discovered during the 1958–1970 Lowell Observatory survey for high proper motion stars in the Northern Hemisphere.[http://adsabs.harvard.edu/abs/1971lpms.book.....G Lowell Proper Motion Survey: 8991 Stars with m > 8, PM > 0.26"/year in the Northern Hemisphere], H. L. Giclas, R. Burnham, Jr., N. G. Thomas, Flagstaff, AZ: Lowell Observatory, 1971. CDS ID [http://vizier.u-strasbg.fr/viz-bin/Cat?I/79 I/79]. Although it did not have high proper motion, it was noticed that it was a very blue star, and hence might be a white dwarf.[http://adsabs.harvard.edu/abs/1967LowOB...7...49G A list of white dwarf suspects II : special objects of small proper motion from the Lowell survey], Henry L. Giclas, Robert Burnham, and Norman Gene Thomas, Bulletin, Lowell Observatory, #141 (7, #4, 1967), pp. 49–54. Greenstein confirmed this in 1969.[http://adsabs.harvard.edu/abs/1969ApJ...158..281G The Lowell Suspect White Dwarfs], Jesse L. Greenstein, Astrophysical Journal 158 (October 1969), pp. 281–293.

In 1968, Arlo U. Landolt discovered the first intrinsically variable white dwarf when he found that HL Tau 76 varied in brightness with a period of approximately 749.5 seconds, or 12.5 minutes.[http://adsabs.harvard.edu/abs/1968ApJ...153..151L A New Short-Period Blue Variable], Arlo U. Landolt, Astrophysical Journal 153, #1 (July 1968), pp. 151–164. By the middle of the 1970s, a number of additional variable white dwarfs had been found, but, like HL Tau 76, they were all white dwarfs of spectral type DA, with hydrogen-dominated atmospheres.[http://adsabs.harvard.edu/abs/1976ApJ...207L..37R Observations of variable white dwarfs: one new variable and 35 nonvariables], E. L. Robinson and J. T. McGraw, Astrophysical Journal 207 (July 1976), pp. L37–L40.[http://adsabs.harvard.edu/abs/1976ApJ...209..853H High-frequency stellar oscillations. XI. The ZZ Ceti star BPM 30551], J. E. Hesser, B. M. Lasker, and H. E. Neupert, Astrophysical Journal 209 (November 1976), pp. 853–857.[http://adsabs.harvard.edu/abs/1976ApJ...210L..35M BPM 31594: a new southern-hemisphere variable white dwarf], J. T. McGraw, Astrophysical Journal 210 (November 1976), pp. L35–L38. In 1982, calculations by Don Winget and his coworkers suggested that helium-atmosphere DB white dwarfs with surface temperatures around 19,000 K should also pulsate.[http://adsabs.harvard.edu/abs/1982ApJ...252L..65W Hydrogen-driving and the blue edge of compositionally stratified ZZ Ceti star models], D. E. Winget, H. M. van Horn, M. Tassoul, G. Fontaine, C. J. Hansen, and B. W. Carroll, Astrophysical Journal 252 (January 15, 1982), pp. L65–L68.^{, p. L67.} Winget then searched for such stars and found that GD 358 was a variable DB, or DBV, white dwarf.{{Cite journal |last1=Winget |first1=D. E. |last2=Robinson |first2=E. L. |last3=Nather |first3=R. E. |author-link3=Ed Nather |last4=Fontaine |first4=G. |date=1982-11-01 |title=Photometric observations of GD 358 : OB white dwarfs do pulsate. |url=https://ui.adsabs.harvard.edu/abs/1982ApJ...262L..11W |journal=The Astrophysical Journal |volume=262 |pages=L11–L15 |doi=10.1086/183902 |bibcode=1982ApJ...262L..11W |issn=0004-637X}} This was the first prediction of a class of variable stars before their observation.White Dwarf Stars, Steven D. Kawaler, in Stellar remnants, S. D. Kawaler, I. Novikov, and G. Srinivasan, edited by Georges Meynet and Daniel Schaerer, Berlin: Springer, 1997. Lecture notes for Saas-Fee advanced course number 25. {{ISBN|3-540-61520-2}}.^{, p. 89.} In 1985, this star was given the variable-star designation V777 Herculis, which is also another name for this class of variable stars.[http://adsabs.harvard.edu/abs/1985IBVS.2681....1K The 67th Name-List of Variable Stars], P. N. Kholopov, N. N. Samus, E. V. Kazarovets, and N. B. Perova, Information Bulletin on Variable Stars, #2681, March 8, 1985.^; White dwarfs, Gilles Fontaine and François Wesemael, in Encyclopedia of Astronomy and Astrophysics, ed. Paul Murdin, Bristol and Philadelphia: Institute of Physics Publishing and London, New York and Tokyo: Nature Publishing Group, 2001. {{ISBN|0-333-75088-8}}.^{, p. 3525}