PG 1159-035

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

{{Starbox begin

| name=PG 1159-035

}}

{{Starbox image

| image = 250px

| caption = A light curve for GW Virginis, adapted from Winget et al. (1985)

}}

{{Starbox observe

| epoch = J2000.0 (ICRS)

| constell = Virgo

| ra = {{RA|12|01|45.9731}}

| dec = {{DEC|−03|45|40.629}}

| appmag_v = 14.9

}}

{{Starbox character

| type = PG 1159

| class = DOQZ1{{cite journal |bibcode=1993PASP..105..761W |title=An Atlas of Optical Spectra of White-Dwarf Stars |last1=Wesemael |first1=F. |last2=Greenstein |first2=J. L. |last3=Liebert |first3=James |last4=Lamontagne |first4=R. |last5=Fontaine |first5=G. |last6=Bergeron |first6=P. |last7=Glaspey |first7=J. W. |journal=Publications of the Astronomical Society of the Pacific |date=1993 |volume=105 |page=761 |doi=10.1086/133228 }}

| variable = GW Vir{{cite journal |bibcode=2017ARep...61...80S |title=General catalogue of variable stars: Version GCVS 5.1 |last1=Samus' |first1=N. N. |last2=Kazarovets |first2=E. V. |last3=Durlevich |first3=O. V. |last4=Kireeva |first4=N. N. |last5=Pastukhova |first5=E. N. |journal=Astronomy Reports |date=2017 |volume=61 |issue=1 |page=80 |doi=10.1134/S1063772917010085 }}

}}

{{Starbox astrometry

| radial_v =

| prop_mo_ra = −14.495

| prop_mo_dec = −3.207

| parallax = 1.6905

| p_error = 0.0642

| parallax_footnote =

| absmag_v =

}}

{{Starbox detail

| mass = 0.63

| temperature = 136,000

| gravity = 7.59

| radius= 0.0254 ± 0.005

| luminosity_bolometric = 200

}}

{{Starbox catalog

| names = GW Vir, GW Virginis, 2E 2572, WD 1159-034{{cite simbad|title=PG 1159-035|access-date=11 June 2007}}

}}

{{Starbox reference

| Simbad = PG%201159-035

}}

{{Starbox end}}

PG 1159-035 is the prototypical PG 1159 star after which the class of PG 1159 stars was named. It was discovered in the Palomar-Green survey of ultraviolet-excess stellar objects and, like the other PG 1159 stars, is in transition between being the central star of a planetary nebula and being a white dwarf.{{cite journal |bibcode=2007A&A...462..281J |title=High-resolution ultraviolet spectroscopy of PG 1159-035 with HST and FUSE |last1=Jahn |first1=D. |last2=Rauch |first2=T. |last3=Reiff |first3=E. |last4=Werner |first4=K. |last5=Kruk |first5=J. W. |last6=Herwig |first6=F. |journal=Astronomy and Astrophysics |year=2007 |volume=462 |issue=1 |page=281 |doi=10.1051/0004-6361:20065901 |arxiv=astro-ph/0610592 |s2cid=17679220 }}

The luminosity of PG 1159-035 was observed to vary in 1979,{{cite journal |bibcode=1979wdvd.coll..377M |title=PG 1159-035: A New, Hot, Non-Da Pulsating Degenerate |last1=McGraw |first1=J. T. |author2-link=Sumner Starrfield |last2=Starrfield |first2=S. G. |last3=Liebert |first3=J. |last4=Green |first4=R. |journal=IAU Colloq. 53: White Dwarfs and Variable Degenerate Stars |year=1979 |page=377 }} and it was given the variable star designation GW Virginis (abbreviation GW Vir) in 1985.{{cite journal |bibcode=1985IBVS.2681....1K |title=The 67th Name-List of Variable Stars |last1=Kholopov |first1=P. N. |last2=Samus |first2=N. N. |last3=Kazarovets |first3=E. V. |last4=Perova |first4=N. B. |journal=Information Bulletin on Variable Stars |year=1985 |volume=2681 |page=1 }} Variable PG 1159 stars may be called GW Vir stars, or the class may be split into DOV and PNNV stars.{{cite journal |bibcode=2004A&A...426L..45N |title=Detection of non-radial g-mode pulsations in the newly discovered PG 1159 star HE 1429-1209 |last1=Nagel |first1=T. |last2=Werner |first2=K. |journal=Astronomy and Astrophysics |year=2004 |volume=426 |doi=10.1051/0004-6361:200400079 |arxiv=astro-ph/0409243 |s2cid=9481357 }}{{cite journal |bibcode=2007ApJS..171..219Q |title=Mapping the Instability Domains of GW vir Stars in the Effective Temperature-Surface Gravity Diagram |last1=Quirion |first1=P. -O |last2=Fontaine |first2=G. |last3=Brassard |first3=P. |journal=The Astrophysical Journal Supplement Series |year=2007 |volume=171 |issue=1 |page=219 |doi=10.1086/513870 |s2cid=122695910 }} The variability of PG 1139-035, like that of other GW Vir stars, arises from non-radial gravity wave pulsations within itself.{{cite journal |doi=10.1088/0953-8984/10/49/014 |title=Asteroseismology of white dwarf stars |year=1998 |last1=Winget |first1=D. E. |journal=Journal of Physics: Condensed Matter |volume=10 |issue=49 |pages=11247–11261 |bibcode=1998JPCM...1011247W |s2cid=250749380 }} Its light curve was observed intensively by the Whole Earth Telescope over a 264-hour period in March 1989, and over 100 of its vibrational modes have been found in the resulting vibrational spectrum, with periods ranging from 300 to 1,000 seconds.{{cite journal |bibcode=1991ApJ...378..326W |title=Asteroseismology of the DOV Star PG 1159-035 with the Whole Earth Telescope |last1=Winget |first1=D. E. |last2=Nather |first2=R. E. |last3=Clemens |first3=J. C. |last4=Provencal |first4=J. |last5=Kleinman |first5=S. J. |last6=Bradley |first6=P. A. |last7=Wood |first7=M. A. |last8=Claver |first8=C. F. |last9=Frueh |first9=M. L. |last10=Grauer |first10=A. D. |last11=Hine |first11=B. P. |last12=Hansen |first12=C. J. |last13=Fontaine |first13=G. |last14=Achilleos |first14=N. |last15=Wickramasinghe |first15=D. T. |last16=Marar |first16=T. M. K. |last17=Seetha |first17=S. |last18=Ashoka |first18=B. N. |last19=O'Donoghue |first19=D. |last20=Warner |first20=B. |last21=Kurtz |first21=D. W. |last22=Buckley |first22=D. A. |last23=Brickhill |first23=J. |last24=Vauclair |first24=G. |last25=Dolez |first25=N. |last26=Chevreton |first26=M. |last27=Barstow |first27=M. A. |last28=Solheim |first28=J. E. |last29=Kanaan |first29=A. |last30=Kepler |first30=S. O. |journal=The Astrophysical Journal |year=1991 |volume=378 |page=326 |doi=10.1086/170434 |hdl=10183/108718 |display-authors=1 |hdl-access=free }}

{{cite journal |bibcode=2008A&A...477..627C |title=The pulsation modes of the pre-white dwarf PG 1159-035 |last1=Costa |first1=J. E. S. |last2=Kepler |first2=S. O. |last3=Winget |first3=D. E. |last4=O'Brien |first4=M. S. |last5=Kawaler |first5=S. D. |last6=Costa |first6=A. F. M. |last7=Giovannini |first7=O. |last8=Kanaan |first8=A. |last9=Mukadam |first9=A. S. |last10=Mullally |first10=F. |last11=Nitta |first11=A. |last12=Provençal |first12=J. L. |last13=Shipman |first13=H. |last14=Wood |first14=M. A. |last15=Ahrens |first15=T. J. |last16=Grauer |first16=A. |last17=Kilic |first17=M. |last18=Bradley |first18=P. A. |last19=Sekiguchi |first19=K. |last20=Crowe |first20=R. |last21=Jiang |first21=X. J. |last22=Sullivan |first22=D. |last23=Sullivan |first23=T. |last24=Rosen |first24=R. |last25=Clemens |first25=J. C. |last26=Janulis |first26=R. |last27=O'Donoghue |first27=D. |last28=Ogloza |first28=W. |last29=Baran |first29=A. |last30=Silvotti |first30=R. |journal=Astronomy and Astrophysics |year=2008 |volume=477 |issue=2 |page=627 |doi=10.1051/0004-6361:20053470 |arxiv=0711.2244 |s2cid=6762152 |display-authors=1 }}