WD 0137−349

Last updated
WD 0137-349
Observation data
Epoch J2000        Equinox J2000
Constellation Sculptor
Right ascension 01h 39m 42.847s [1]
Declination −34° 42′ 39.32″ [1]
Apparent magnitude  (V)+15.33 ± 0.02 [2]
Characteristics
Spectral type DA [3] + L8 [2] /T [4]
B−V color index −0.02
Astrometry
Proper motion (μ)RA: -42.059 [5]   mas/yr
Dec.: -48.895 [5]   mas/yr
Parallax (π)9.8472 ± 0.0367  mas [5]
Distance 331 ± 1  ly
(101.6 ± 0.4  pc)
Orbit [6]
Period (P)0.0803 ± 0.0002
Semi-major axis (a)0.65 R☉
Periastron epoch (T)2453686.5276 ± 0.0001
Semi-amplitude (K1)
(primary)		27.9 ± 0.3 km/s
Semi-amplitude (K2)
(secondary)		−187.5 ± 1.1 km/s
Details
WD 0137-349A
Mass 0.39 ± 0.035 [6]   M☉
Radius 0.0186 ± 0.0012 [6]   R☉
Luminosity 0.023 ± 0.004 [6]   L☉
Surface gravity (log g)7.49 ± 0.08 [6]   cgs
Temperature 16500 ± 500 [6]   K
Age 250 ± 80 [6]   Myr
WD 0137-349B
Mass 0.053 ± 0.006 [2]   M☉
Temperature 1300 to 1400 [2]   K
Other designations
2MASS J01394284-3442393, BPS CS 29504-0036 [7]
Database references
SIMBAD A
B

WD 0137-349 is a binary star in the constellation of Sculptor. It is located about 330 light-years (100 parsecs) away, and appears exceedingly faint with an apparent magnitude of 15.33. [2]

Contents

It is composed of a white dwarf with a brown dwarf in orbit around it, and is one of the few systems composed of a white dwarf and an associated brown dwarf. [6] The brown dwarf orbits with a period of 116 minutes, or nearly 2 hours. [6]

Properties

The primary is a typical hydrogen white dwarf, as indicated by its spectral type of DA. It has about 39% of the Sun's mass and is only 1.86% as wide (12,900 km). [6] With a high effective temperature of 16,500 K, it emits radiation mostly in the ultraviolet range. [8]

The brown dwarf, designated WD 0137-349B, can be detected from an infrared excess. [2] Although it glows with an effective temperature of 1300 to 1400 K, the side facing the white dwarf's intercepts 1% of its light, and heats it up to around 2000 K. [8] The "night" side spectrum of WD 0137-349B therefore matches that of a mid-T-type brown dwarf, while the "day" side spectrum matches that of an early L-type brown dwarf. [4] The brown dwarf is suspected to be a white dwarf or even a strange star, as a hydrogen-dominated substellar object may be unstable in such a small orbit. [9]

Evolution

The brown dwarf is known to have survived being engulfed when the primary star was a red giant, [6] because it was relatively massive. At that time, the red giant had a radius of 100 R☉. [10] It is thought that the red giant phase of the current white dwarf was shortened from around 100 million years on average, to a few decades—while the brown dwarf was within the red giant, it hastened the expulsion of matter during this phase by rapidly heating gas and accreting a portion of it. During this phase, drag from the red giant also decreased the orbital speed of the brown dwarf, causing it to fall inwards. [11]

The orbit of the brown dwarf is slowly decaying. [6] In about 1.4 billion years, it is thought that the orbit of the brown dwarf will have decayed sufficiently to allow the white dwarf to draw matter away and accrete it on its surface, leading to a cataclysmic variable. [6]

As of 2006, this is the coldest known companion to a white dwarf. [2] This brown dwarf was also the object with the lowest mass known to have survived being engulfed by a red giant. Previously, only red dwarfs had been known to survive being enveloped during a red giant phase. It is thought that objects smaller than 20 Jupiter masses would have evaporated. [11]

Post common envelope white dwarf-brown dwarf binaries

WD 0137-349 represents the first confirmed post common envelope binary (PCEB) containing a white dwarf and a brown dwarf. As of 2018 only 8 of these wd+bd PCEBs are known. The first with a confirmed spectral type was GD 1400, but this second confirmed wd+bd binary after GD 165B [12] was confirmed as a PCEB in 2011, five years later than WD 0137-349. [13]

Related Research Articles

<span class="mw-page-title-main">White dwarf</span> Type of stellar remnant composed mostly of electron-degenerate matter

A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: its mass is comparable to the Sun's, while its volume is comparable to the Earth's. A white dwarf's low luminosity comes from the emission of residual thermal energy; no fusion takes place in a white dwarf. The nearest known white dwarf is Sirius B, at 8.6 light years, the smaller component of the Sirius binary star. There are currently thought to be eight white dwarfs among the hundred star systems nearest the Sun. The unusual faintness of white dwarfs was first recognized in 1910. The name white dwarf was coined by Willem Luyten in 1922.

<span class="mw-page-title-main">Brown dwarf</span> Type of substellar object larger than a planet

Brown dwarfs are substellar objects that have more mass than the biggest gas giant planets, but less than the least massive main-sequence stars. Their mass is approximately 13 to 80 times that of Jupiter (MJ) -- not big enough to sustain nuclear fusion of ordinary hydrogen (1H) into helium in their cores, but massive enough to emit some light and heat from the fusion of deuterium (2H). The most massive ones can fuse lithium (7Li).

<span class="mw-page-title-main">Crater (constellation)</span> Constellation in the southern celestial hemisphere

Crater is a small constellation in the southern celestial hemisphere. Its name is the latinization of the Greek krater, a type of cup used to water down wine. One of the 48 constellations listed by the second-century astronomer Ptolemy, it depicts a cup that has been associated with the god Apollo and is perched on the back of Hydra the water snake.

<span class="mw-page-title-main">Binary pulsar</span> Two pulsars orbiting each other

A binary pulsar is a pulsar with a binary companion, often a white dwarf or neutron star. Binary pulsars are one of the few objects which allow physicists to test general relativity because of the strong gravitational fields in their vicinities. Although the binary companion to the pulsar is usually difficult or impossible to observe directly, its presence can be deduced from the timing of the pulses from the pulsar itself, which can be measured with extraordinary accuracy by radio telescopes.

<span class="mw-page-title-main">Zeta Cygni</span> Star in the constellation Cygnus

Zeta Cygni is a binary star system in the northern constellation of Cygnus, the swan. It has an apparent visual magnitude of 3.26 and, based upon parallax measurements, is about 143 light-years away.

<span class="mw-page-title-main">NN Serpentis</span> Eclipsing post-common envelope binary star system in the constellation Serpens

NN Serpentis is an eclipsing post-common envelope binary system approximately 1670 light-years away. The system comprises an eclipsing white dwarf and red dwarf. The two stars orbit each other every 0.13 days.

Blanco 1 is a nearby open cluster of stars located around 850 light years away from the Sun in the southern constellation of Sculptor near the star ζ Sculptoris. It was discovered by Puerto Rican astronomer Víctor Manuel Blanco in 1949, who noticed an unusually high proportion of A-type stars in an area spanning 1.5°. This cluster is relatively young, with an age of about 100–150 million years. It is positioned at a high galactic latitude of b = –79.3° and is located some 780 ly (240 pc) below the galactic plane.

2MASS J03552337+1133437 is a nearby brown dwarf of spectral type L5γ, located in constellation Taurus at approximately 29.8 light-years from Earth.

<span class="mw-page-title-main">RR Caeli</span> Double star in the constellation Caelum

RR Caeli is an eclipsing binary star in the constellation Caelum. It is 69 light years from Earth.

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<span class="mw-page-title-main">Post common envelope binary</span> Binary system consisting of a white dwarf and a main sequence star or a brown dwarf

A post-common envelope binary (PCEB) or pre-cataclysmic variable is a binary system consisting of a white dwarf or hot subdwarf and a main-sequence star or a brown dwarf. The star or brown dwarf shared a common envelope with the white dwarf progenitor in the red giant phase. In this scenario the star or brown dwarf loses angular momentum as it orbits within the envelope, eventually leaving a main-sequence star and white dwarf in a short-period orbit. A PCEB will continue to lose angular momentum via magnetic braking and gravitational waves and will eventually begin mass-transfer, resulting in a cataclysmic variable. While there are thousands of PCEBs known, there are only a few eclipsing PCEBs, also called ePCEBs. Even more rare are PCEBs with a brown dwarf as the secondary. A brown dwarf with a mass lower than 20 MJ might evaporate during the common envelope phase and therefore the secondary is supposed to have a mass higher than 20 MJ.

<span class="mw-page-title-main">WD 1856+534</span> White dwarf located in the constellation Draco

WD 1856+534 is a white dwarf located in the constellation of Draco. At a distance of about 25 parsecs (80 ly) from Earth, it is the outer component of a visual triple star system consisting of an inner pair of red dwarf stars. The white dwarf displays a featureless absorption spectrum, lacking strong optical absorption or emission features in its atmosphere. It has an effective temperature of 4,700 K, corresponding to an age of approximately 5.8 billion years. WD 1856+534 is approximately half as massive as the Sun, while its radius is much smaller, being 40% larger than Earth.

HD 136138, or HR 5692, is a binary star system in the Serpens Caput segment of the Serpens constellation. It has a golden hue like the Sun and is dimly visible to the naked eye with an apparent visual magnitude of 5.68; the light contribution from the companion is effectively negligible. This system is located at a distance of approximately 420 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −7.7 km/s and has a proper motion of 23.5 mas·yr−1.

WASP-84, also known as BD+02 2056, is a G-type main-sequence star 327 light-years away in the constellation Hydra. Its surface temperature is 5350±31 K and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. WASP-84's age is probably older than the Sun at 8.5+4.1
−5.5 billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.

NGTS-1 is a solitary red dwarf located in the constellation Columba (constellation). With an apparent magnitude of 15.52, it requires a powerful telescope to be seen. The star is located 716 light years away from the Solar System, and is drifting away with a high radial velocity of 97.2 km/s (60.4 mi/s).

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

<span class="mw-page-title-main">V471 Tauri</span> Variable star in the constellation Taurus

V471 Tauri is a eclipsing variable star in the constellation of Taurus. The star has a visual magnitude of 9 which makes it impossible to see with the naked eye. It is around 155 light-years away from the Solar System.

References

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  2. 1 2 3 4 5 6 7 Burleigh, M. R.; Hogan, E.; Dobbie, P. D.; Napiwotzki, R.; Maxted, P. F. L. (2006). "A near-infrared spectroscopic detection of the brown dwarf in the post common envelope binary WD 0137-349". Monthly Notices of the Royal Astronomical Society: Letters. 373 (1): L55–L59. arXiv: astro-ph/0609366 . Bibcode:2006MNRAS.373L..55B. doi:10.1111/j.1745-3933.2006.00242.x. S2CID   16186119.
  3. ↑ Koester, D.; Voss, B.; Napiwotzki, R.; Christlieb, N.; Homeier, D.; Lisker, T.; Reimers, D.; Heber, U. (2009). "High-resolution UVES/VLT spectra of white dwarfs observed for the ESO SN Ia Progenitor Survey" (PDF). Astronomy and Astrophysics. 505 (1): 441–462. arXiv: 0908.2322 . Bibcode:2009A&A...505..441K. doi:10.1051/0004-6361/200912531. S2CID   10435049.
  4. 1 2 Zhou, Yifan; Apai, Dániel; Tan, Xianyu; Lothringer, Joshua D.; Lew, Ben W. P.; Casewell, Sarah L.; Parmentier, Vivien; Marley, Mark S.; Xu, Siyi; Mayorga, L. C. (2022). "HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122". The Astronomical Journal. 163 (1): 17. arXiv: 2110.10162 . Bibcode:2022AJ....163...17Z. doi: 10.3847/1538-3881/ac3095 . S2CID   239050135.
  5. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  6. 1 2 3 4 5 6 7 8 9 10 11 12 13 Maxted, P. F. L.; Napiwotzki, R.; Dobbie, P. D.; Burleigh, M. R. (2006). "Survival of a brown dwarf after engulfment by a red giant star". Nature. 442 (7102): 543–5. arXiv: astro-ph/0608054 . Bibcode:2006Natur.442..543M. doi:10.1038/nature04987. PMID   16885979. S2CID   4368344.
  7. ↑ "BPS CS 29504-0036". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 16 April 2017.
  8. 1 2 Casewell, S. L.; Lawrie, K. A.; Maxted, P. F. L.; Marley, M. S.; Fortney, J. J.; Rimmer, P. B.; Littlefair, S. P.; Wynn, G.; Burleigh, M. R.; Helling, C. (2015). "Multiwaveband photometry of the irradiated brown dwarf WD0137-349B". Monthly Notices of the Royal Astronomical Society. 447 (4): 3218. arXiv: 1412.6363 . Bibcode:2015MNRAS.447.3218C. doi:10.1093/mnras/stu2721. S2CID   46597477.
  9. ↑ Kuerban, Abudushataer; Geng, Jin-Jun; Huang, Yong-Feng; Zong, Hong-Shi; Gong, Hang (2020), "Close-in Exoplanets as Candidates for Strange Quark Matter Objects", The Astrophysical Journal, 890 (1): 41, arXiv: 1908.11191 , Bibcode:2020ApJ...890...41K, doi: 10.3847/1538-4357/ab698b , S2CID   201671383
  10. ↑ Passy, Jean-Claude; Mac Low, Mordecai-Mark; De Marco, Orsola (2012). "On the Survival of Brown Dwarfs and Planets Engulfed by Their Giant Host Star". The Astrophysical Journal. 759 (2): L30. arXiv: 1210.0879 . Bibcode:2012ApJ...759L..30P. doi:10.1088/2041-8205/759/2/L30. S2CID   118657091.
  11. 1 2 Ker Than (2 August 2006). "Object Survives Being Swallowed by a Star". Space.com. Retrieved 19 April 2017.
  12. ↑ Farihi, J.; Christopher, M. (October 2004). "A Possible Brown Dwarf Companion to the White Dwarf GD 1400". The Astronomical Journal. 128 (4): 1868–1871. arXiv: astro-ph/0407036 . Bibcode:2004AJ....128.1868F. doi:10.1086/423919. ISSN   0004-6256. S2CID   119530628.
  13. ↑ Casewell, S. L.; Braker, I. P.; Parsons, S. G.; Hermes, J. J.; Burleigh, M. R.; Belardi, C.; Chaushev, A.; Finch, N. L.; Roy, M.; Littlefair, S. P.; Goad, M. (2018-05-01). "The first sub-70 minute non-interacting WD-BD system: EPIC212235321". Monthly Notices of the Royal Astronomical Society. 476 (1): 1405–1411. arXiv: 1801.07773 . Bibcode:2018MNRAS.476.1405C. doi: 10.1093/mnras/sty245 . ISSN   0035-8711.
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