Wolf 1061

Last updated

Wolf 1061
Wolf 1061-starmap.png
Location of Wolf 1061 in the constellation Ophiuchus
Observation data
Epoch J2000       Equinox J2000
Constellation Ophiuchus
Right ascension 16h 30m 18.0584s [1]
Declination −12° 39′ 45.325″ [1]
Apparent magnitude  (V)10.07 [2] (10.05 - 10.10) [3]
Characteristics
Spectral type M3.5V [4]
U−B color index +1.20 [5]
B−V color index +1.57 [2]
Variable type BY Draconis [3]
Astrometry
Radial velocity (Rv)−21.22 [6]  km/s
Proper motion (μ)RA: −94.212 [1]   mas/yr
Dec.: 1,183.679 [1]   mas/yr
Parallax (π)232.1390 ± 0.0268  mas [7]
Distance 14.050 ± 0.002  ly
(4.3078 ± 0.0005  pc)
Absolute magnitude  (MV)11.87 [4]
Details
Mass 0.304±0.007 [8]   M☉
Radius 0.319±0.007 [8]   R☉
Luminosity (bolometric)0.0110±0.0001 [8]   L☉
Luminosity (visual, LV)0.0015  L☉
Temperature 3,307+38
−36 [8]   K
Metallicity [Fe/H]−0.09±0.09 [4]   dex
Rotation 95 d [4]
Other designations
BD−12°4523, G 153-058, GCTP 3746.00, GJ 628, HIP 80824, LHS 419, Vys 164
Database references
SIMBAD data

Wolf 1061 (also known as HIP 80824 and V2306 Ophiuchi) is an M-class red dwarf star located about 14.1 light-years away in the constellation Ophiuchus. It is the 36th-closest-known star system to the Sun and has a relatively high proper motion of 1.2 seconds of arc per year. Wolf 1061 does not have any unusual spectroscopic features. [9]

Contents

The star

A visual band light curve for V2306 Ophiuchi, plotted from ASAS-SN data V2306OphLightCurve.png
A visual band light curve for V2306 Ophiuchi, plotted from ASAS-SN data

Wolf 1061 was first cataloged in 1919 by German astronomer Max Wolf when he published a list of dim stars that had high proper motions. Wolf 1061's name originates from this list. [11] A seven years study found no evidence of photometric transits and confirms the radial velocity signals are not due to stellar activity. The habitable zone estimate for the system lies between approximately 0.1 and 0.2 AU from the star.

Planetary system

Artist's impression of exoplanets orbiting a red dwarf Planets Under a Red Sun.jpg
Artist's impression of exoplanets orbiting a red dwarf

In December 2015, a team of astronomers from the University of New South Wales announced the discovery of three planets orbiting Wolf 1061. The planets were detected by analyzing 10 years of observations of the Wolf 1061 system by the HARPS spectrograph at La Silla Observatory in Chile. The team used archive radial velocity measurements of the star's spectrum in the HARPS data and, along with 8 years of photometry from the All Sky Automated Survey, discovered two definite planets with orbital periods of around 4.9 and 17.9 days and a very likely third with a period of 67.3 days. [9]

All three planets have masses low enough that they are likely to be rocky planets similar to the inner planets of the Solar System although their actual sizes and densities are currently unknown. However, this information could be determined if the planets happen to transit in front of Wolf 1061 when viewed from Earth. Because all three planets orbit close to the star and have short orbital periods, there is a chance that this will occur. The University of New South Wales team estimated the chances of a transit at around 14% for planet b, 6% for planet c, and 3% for planet d. [9]

One of the planets, Wolf 1061 c, is a super-Earth located near the inner edge of the star's habitable zone, which conservatively extends from 0.11 to 0.21 AU, or at most from 0.09 to 0.23 AU. [2] It is one of the closest known potentially habitable planets to Earth after Proxima b, Ross 128 b, and Luyten b. [13] [14] The next planet out, Wolf 1061 d, could be marginally habitable depending on its atmosphere's composition as it orbits just beyond the habitable zone. [9]

In March 2017, another team of astronomers re-analyzed the system using the HARPS spectrograph. They found planets b and c to be quite similar to their originally reported parameters, but found that planet d was more massive and in a larger, more eccentric orbit. The team was also able to find updated parameters for the host star. Their results showed that Wolf 1061 c is slightly smaller, yet closer to the inner edge of the habitable zone. [4]

The Wolf 1061 planetary system [9] [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥1.91 ± 0.25  M🜨 0.0375 ± 0.00124.8869 ± 0.00050.15 +0.13
−0.10		—1.2 (estimated)  R🜨
c ≥3.41 +0.43
−0.41  M🜨 		0.0890 ± 0.00317.8719 ± 0.00590.11 +0.10
−0.07		—1.45 (estimated)  R🜨
d ≥7.7 +1.12
−1.06  M🜨 		0.470 ± 0.016217.21 +0.55
−0.52		0.55 +0.08
−0.09		—2.2 (estimated)  R🜨

See also

Related Research Articles

GJ 1061 is a red dwarf star located 12 light-years from Earth in the southern constellation of Horologium. Even though it is a relatively nearby star, it has an apparent visual magnitude of about 13, so it can only be seen with at least a moderately-sized telescope.

Luyten's Star (GJ 273) is a red dwarf in the constellation Canis Minor located at a distance of approximately 12.35 light-years from the Sun. It has a visual magnitude of 9.9, making it too faint to be viewed with the unaided eye. It is named after Willem Jacob Luyten, who, in collaboration with Edwin G. Ebbighausen, first determined its high proper motion in 1935. The star has two confirmed planets and two candidate planets, of which Luyten b is in the circumstellar habitable zone.

<span class="mw-page-title-main">Gliese 876</span> Star in the constellation Aquarius

Gliese 876 is a red dwarf star 15.2 light-years away from Earth in the constellation of Aquarius. It is one of the closest known stars to the Sun confirmed to possess a planetary system with more than two planets, after GJ 1061, YZ Ceti, Tau Ceti, and Wolf 1061; as of 2018, four extrasolar planets have been found to orbit the star. The planetary system is also notable for the orbital properties of its planets. It is the only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of Laplace resonance. It is also the first extrasolar system around a normal star with measured coplanarity. While planets b and c are located in the system's habitable zone, they are giant planets believed to be analogous to Jupiter.

<span class="mw-page-title-main">Gliese 229</span> Star in the constellation Lepus

Gliese 229 is a binary system composed of a red dwarf and the first brown dwarf seen by astronomers, 18.8 light years away in the constellation Lepus. The primary component has 58% of the mass of the Sun, 69% of the Sun's radius, and a very low projected rotation velocity of 1 km/s at the stellar equator.

HD 147513 is a star in the southern constellation of Scorpius. It was first catalogued by Italian astronomer Piazzi in his star catalogue as "XVI 55". With an apparent magnitude of 5.38, according to the Bortle scale it is visible to the naked eye from suburban skies. Based upon stellar parallax measurements by the Hipparcos spacecraft, HD 147513 lies some 42 light years from the Sun.

<span class="mw-page-title-main">Groombridge 34</span> Binary star system in the constellation of Andromeda

Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years from the Sun. This positions the pair among the nearest stars to the Solar System.

TZ Arietis is a red dwarf in the northern constellation of Aries. With a normal apparent visual magnitude of 12.3, it is too faint to be seen by the naked eye, although it lies relatively close to the Sun at a distance of 14.6 light-years. It is a flare star, which means it can suddenly increase in brightness for short periods of time.

Gliese 674(GJ 674) is a small red dwarf star with an exoplanetary companion in the southern constellation of Ara. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.38 and an absolute magnitude of 11.09. The system is located at a distance of 14.8 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −2.9 km/s. It is a candidate member of the 200 million year old Castor stream of co-moving stars.

<span class="mw-page-title-main">Gliese 105</span> Triple star system in the constellation Cetus

Gliese 105 is a triple star system in the constellation of Cetus. It is located relatively near the Sun at a distance of 23.6 light-years. Despite this, even the brightest component is barely visible with the unaided eye (see Bortle scale). No planets have yet been detected around any of the stars in this system.

Gliese 832 is a red dwarf of spectral type M2V in the southern constellation Grus. The apparent visual magnitude of 8.66 means that it is too faint to be seen with the naked eye. It is located relatively close to the Sun, at a distance of 16.2 light years and has a high proper motion of 818.16 milliarcseconds per year. Gliese 832 has just under half the mass and radius of the Sun. Its estimated rotation period is a relatively leisurely 46 days. The star is roughly 6 billion years old.

Gliese 682 or GJ 682 is a red dwarf. It is listed as the 53rd-nearest known star system to the Sun, being 16.3 light years away from the Earth. Even though it is close by, it is dim with a magnitude of 10.95 and thus requires a telescope to be seen. It is located in the constellation of Scorpius, near the bright star Theta Scorpii. The star is in a crowded region of sky near the Galactic Center, and so appears to be near a number of deep-sky objects from the Solar System's perspective. The star is only 0.5 degrees from the much more distant globular cluster NGC 6388.

<span class="mw-page-title-main">Gliese 752</span> Binary star system in the constellation Aquila

Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of about 19 light years.

Gliese 163 is a faint red dwarf star with multiple exoplanetary companions in the southern constellation of Dorado. Other stellar catalog names for it include HIP 19394 and LHS 188. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 11.79 and an absolute magnitude of 10.91. This system is located at a distance of 49.4 light-years from the Sun based on parallax measurements. Judging by its space velocity components, it is most likely a thick disk star.

<span class="mw-page-title-main">Gliese 180</span> Star in the constellation Eridanus

Gliese 180, is a small red dwarf star in the equatorial constellation of Eridanus. It is invisible to the naked eye with an apparent visual magnitude of 10.9. The star is located at a distance of 39 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −14.6 km/s. It has a high proper motion, traversing the sky at the rate of 0.765 arcseconds per year.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

GJ 625 is a small red dwarf star with an exoplanetary companion in the northern constellation of Draco. The system is located at a distance of 21.1 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 10.13 and an absolute magnitude of 11.06.

GJ 1132 is a small red dwarf star 41.1 light-years away from Earth in the constellation Vela. In 2015, it was revealed to have a hot rocky Earth-sized planet orbiting it every 1.6 days. In 2018, a second planet and a potential third were revealed.

<span class="mw-page-title-main">Gliese 357</span>

GJ 357 is an M-type main sequence star with an unusually low starspot activity. It is located 31 light-years from the Solar System. The system is part of the Hydra constellation.

References

  1. 1 2 3 4 Gaia Collaboration; Brown, A. G. A; Vallenari, A; Prusti, T; De Bruijne, J. H. J; Mignard, F; Drimmel, R; Babusiaux, C; Bailer-Jones, C. A. L; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics. 595: A2. arXiv: 1609.04172 . Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. S2CID   1828208.
  2. 1 2 3 Kane, Stephen R.; et al. (February 2017), "Characterization of the Wolf 1061 Planetary System", The Astrophysical Journal, 835 (2): 9, arXiv: 1612.09324 , Bibcode:2017ApJ...835..200K, doi:10.3847/1538-4357/835/2/200, S2CID   30738573, 200.
  3. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. 1 2 3 4 5 6 Astudillo-Defru, Nicola; Forveille, Thierry; Bonfils, Xavier; Ségransan, Damien; Bouchy, François; Delfosse, Xavier; et al. (2017). "The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293". Astronomy and Astrophysics. 602. A88. arXiv: 1703.05386 . Bibcode:2017A&A...602A..88A. doi:10.1051/0004-6361/201630153. S2CID   119418595.
  5. ↑ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
  6. ↑ Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv: astro-ph/0112477 , Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID   51814894.
  7. ↑ 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.
  8. 1 2 3 4 Pineda, J. Sebastian; et al. (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv: 2106.07656 . Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID   235435757. 40.
  9. 1 2 3 4 5 Wright, D. J; Wittenmyer, R. A; Tinney, C. G; Bentley, J. S; Zhao, Jinglin (2016). "Three Planets Orbiting Wolf 1061". The Astrophysical Journal Letters. 817 (2): L20. arXiv: 1512.05154 . Bibcode:2016ApJ...817L..20W. doi:10.3847/2041-8205/817/2/L20. S2CID   52320394.
  10. ↑ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
  11. ↑ Wolf, M. (June 1919). "Katalog von 1053 staerker bewegten Fixsternen (Catalog of 1053 moving fixed stars)". Veroeffentlichungen der Badischen Sternwarte zu Heidelberg (in German). 7 (10): 195–219. Bibcode:1919VeHei...7..195W.
  12. ↑ "Astronomers discover closest potentially habitable planet: Wolf 1061c". ScienceAlert.com. 17 December 2015. Retrieved 17 December 2015.
  13. ↑ Davison, Cassy L.; White, Russel J.; Henry, Todd J.; Riedel, Adric R.; Jao, Wei-Chun; Bailey III, John I.; Quinn, Samuel N.; Justin R., Cantrell; John P., Subasavage; Jen G., Winters (2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs". The Astronomical Journal. 149 (3): 106. arXiv: 1501.05012 . Bibcode:2015AJ....149..106D. doi:10.1088/0004-6256/149/3/106. S2CID   9719725.
  14. ↑ Stuart Gary (17 December 2015). "Potentially habitable super-Earth discovered orbiting star 14 light years from Earth". ABC News (Australia).
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.