Jump to content

Wolf 359

Coordinates:Sky map10h56m28.99s,+07° 00′ 52″
This is a good article. Click here for more information.
From Wikipedia, the free encyclopedia
This article is about the star. For the fictional battle, seeThe Best of Both Worlds (Star Trek: The Next Generation).ForThe Outer Limitsepisode, seeWolf 359 (The Outer Limits).For the podcast, seeWolf 359(podcast).
Wolf 359

Wolf 359 is the orange-hued star located just above the center of this 2009astrophotograph.
Observation data
EpochJ2000EquinoxJ2000
Constellation Leo
Right ascension 10h56m28.92087s[1]
Declination +07° 00′ 53.0033″[1]
Apparent magnitude(V) 13.507[2]
Characteristics
Spectral type M6V[3]
Apparent magnitude(J) 7.1[4]
Apparent magnitude(K) 6.1[4]
U−Bcolor index +1.165[2]
B−Vcolor index +2.034[2]
Variable type UV Ceti[5]
Astrometry
Radial velocity(Rv)+19±1[6]km/s
Proper motion(μ)RA:−3,866.338mas/yr[1]
Dec.:−2,699.215mas/yr[1]
Parallax(π)415.1794 ± 0.0684mas[1]
Distance7.856 ± 0.001ly
(2.4086 ± 0.0004pc)
Absolute magnitude(MV)16.614[7]
Details
Mass0.110±0.003[8]M☉
Radius0.144±0.004[8]R☉
Luminosity0.00106 ± 0.00002[8]L☉
Habitable zoneinner limit0.024[9]AU
Habitable zoneouter limit0.052[9]AU
Surface gravity(logg)5.5[10]cgs
Temperature2,749+44
−41[8]K
Metallicity[Fe/H]+0.25[11]dex
Rotation2.704±0.003d[12]
Rotational velocity(vsini)2.9±0.8[13]km/s
Age0.1-1.5[14]Gyr
Other designations
CN Leonis, CN Leo,GJ406,G045-020,LTT12923, LFT 750,LHS36,GCTP2553[15]
Database references
SIMBADdata
Wolf 359 is located in the constellation Leo.
Wolf 359 is located in the constellation Leo.
Wolf 359
Wolf 359 is shown near the ecliptic in the southern region ofLeo.

Wolf 359is ared dwarfstar located in the constellationLeo,near theecliptic.At a distance of 7.86light-years(2.41parsecs) fromEarth,it has anapparent magnitudeof 13.54 and can only be seen with a largetelescope.Wolf 359 is one of thenearest starsto theSun;only theAlpha Centaurisystem (includingProxima Centauri),Barnard's Star,and thebrown dwarfsLuhman 16(WISE 1049-5319) andWISE 0855−0714are known to be closer. Its proximity to Earth has led to its mention in several works of fiction.[citation needed][16]

Wolf 359 is one of the faintest and least-massive nearby stars known. At the light-emitting layer called thephotosphere,it has a temperature of ~2,800K,low enough forchemical compoundsto form and survive. Theabsorption linesof compounds such as water andtitanium(II) oxidehave been observed in itsspectrum.[17]The star's surface has amagnetic fieldhundreds of times as strong as that of theSun,generated by its thorough internalconvection.As a result of this significant magnetic activity, Wolf 359 is aflare starthat can undergo sudden and great increases in luminosity, which can persist for several minutes. These flares emit strong bursts ofX-rayandgamma rayradiation that have been observed byspace telescopes.It is a relatively young star with an estimated age of less than a billion years. No planetary companions for Wolf 359 have been confirmed so far, though there is one unverified candidate, and as yet nodebris diskshave been found.[14]

Observation history and name

[edit]

Wolf 359 first came to the attention of astronomers because of its relatively high rate oftransversemotion against the background, also known as theproper motion.A high rate of proper motion can indicate that the star is located nearby, as closer stars can achieve the same rate of angular change with a lower relative speed. The proper motion of Wolf 359 was first measured in 1917 by GermanastronomerMax Wolf,aided byastrophotography.In 1919 he published a catalogue of over one thousand stars with highproper motions,including this one, that are still identified by his name.[18]He listed this star as entry number 359, and the star has since been referred to as Wolf 359, in reference to Max Wolf's work.[19]

The firstparallaxmeasurement of Wolf 359 was reported in 1928 from theMount Wilson Observatory,yielding an annual shift in the star's position of0.407 ± 0.009arcseconds.From this position change, and the known size of the Earth's orbit, the distance to the star could be estimated. It was the faintest and least-massive star known until the discovery ofVB 10in 1944.[20][21]Theinfraredmagnitude of the star was measured in 1957.[22]In 1969, a brief flare in the luminosity of Wolf 359 was observed, linking it to a class ofvariable starsknown asflare stars.[23]

Properties

[edit]
The position of Wolf 359 on aradarmap among all stellar objects orstellar systemswithin 9 light years (ly) from the map's center, the Sun (Sol). The diamond-shapes are their positions entered according toright ascensioninhours angle(indicated at the edge of the map's reference disc), and according to theirdeclination.The second mark shows each's distance from Sol, with theconcentriccircles indicating the distance in steps of one ly.

Wolf 359 has astellar classificationof M6,[3]although various sources list a spectral class of M5.5,[24]M6.5[25]or M8.[26]MostM-type starsarered dwarfs:they are visually red because the energy emission of such stars reaches a peak in the red and infrared parts of the spectrum.[27]Wolf 359 has a very low luminosity, emitting about 0.1% of theSun's power.[28][8]If it were moved to the location of the Sun, it would appear ten times as bright as thefull Moon.[29]

At an estimated 11% of theSun's mass,Wolf 359 is just above the lower limit at which a star's core can undergohydrogen fusionthrough theproton–proton chain reaction:~8% of the solar mass.[30](Substellar objectsbelow this limit are known asbrown dwarfs.) The radius of Wolf 359 is an estimated 14.4%that of the Sun,[8]or about100,200km.[31]For comparison, the equatorial radius of the planetJupiteris71,490 km,making the star a mere 40% wider than the planet.[32]

The entire starundergoes convection,whereby the energy generated at the core is transported toward the surface by the convective motion of stellarplasma,rather than throughelectromagnetic radiation.This constant circulation redistributes throughout the star any excess accumulation of helium in the core generated bystellar nucleosynthesis.[33]This process allows Wolf 359 to remain on themain sequenceas ahydrogenfusing star for proportionately longer than one such as the Sun, for which helium steadily accumulates in the core and is not diluted. In conjunction with a much lower rate of hydrogen consumption due to its low mass and core temperature, Wolf 359 is expected to remain a main sequence star for about eight trillion years before finally exhausting its hydrogen supply and ending up as a heliumwhite dwarf.[34]

A search of this star by theHubble Space Telescoperevealed no stellar companions.[35]Noexcess infrared emissionhas been detected, which may indicate the lack of adebris diskaround it.[36][37]

Outer atmosphere

[edit]

The outer, light-emitting layer of a star is known as thephotosphere.Estimates of the photospheric temperature of Wolf 359 range from 2,500 K to 2,900 K,[38]which is sufficiently cool forequilibrium chemistryto occur. The resultingchemical compoundssurvive long enough to be observed through theirspectral lines.[39]Numerousmolecularbands appear in the spectrum of Wolf 359, including those ofcarbon monoxide(CO),[40]iron hydride(FeH),chromiumhydride (CrH), water (H2O),[17]magnesiumhydride (MgH),vanadium(II) oxide(VO),[28]titanium(II) oxide(TiO), and possibly the molecule CaOH.[41]Since there are no lines oflithiumin the spectrum, this element must have already been consumed by fusion in the core. This indicates that the star must be at least 100 million years old.[28]

Beyond the photosphere lies a nebulous, high temperature region known as thestellar corona.In 2001, Wolf 359 became the first star other than the Sun to have the spectrum of its corona observed by a ground-based telescope. The spectrum showedemission linesof Fe XIII, which is heavilyionizediron that has been stripped of twelve of its electrons.[42]The strength of this line can vary over a time period of several hours, which may be evidence ofmicroflareheating.[28]

Ablue bandlight curvefor a flare of CN Leonis, adapted from Liefkeet al.(2007)[43]

Wolf 359 is classified as aUV Ceti-typeflare star,[5]a category of stars that undergo brief, dramatic increases in luminosity due to intense magnetic field activity in their photospheres. Itsvariable star designationisCN Leonis.Wolf 359 has a relatively high flare rate. Observations with the Hubble Space Telescope detected 32 flare events within a two-hour period, with energies of 1027ergs(1020joules) and higher.[26]The mean magnetic field strength at the surface of the star is around 2.2kG(0.22teslas), but this value varies significantly on time scales as short as six hours.[24]In comparison, the magnetic field of the Sun averages a strength of 1 gauss (100μT), although it can reach as high as 3 kG (0.3 T) in activesunspotregions.[44]During periods of flare activity, Wolf 359 has been observed to emitX-raysandgamma rays.[45][46]

Motion

[edit]
Distances of thenearest starsfrom 20,000 years ago to 80,000 years in the future. Wolf 359 is not displayed, but it is currently at a distance of 7.9 ly and increasing, with a past minimum of 7.3 ly around 13,850 years ago.

The rotation of a star causes aDoppler shiftof its spectrum, generally resulting in a broadening of theabsorption linesin its spectrum, with the lines increasing in width with higher rotational speeds. However, only the rotational velocity's component in the direction of the observer can be measured by this method, and the resulting data imposes only a lower limit on the star's rotational speed. This projectedrotational velocityof Wolf 359 at its equator is less than 3 km/s, below the threshold of detection withspectral line broadening.[6]This low rate of rotation may have been caused by the loss ofangular momentumthrough itsstellar wind,which increases greatly during periods of flare activity. Roughly speaking, the spin-down timescale of a star of spectral class M6 is somewhat long, at ~10 billion years, as fully convective stars lose their rotational speeds more slowly than others.[47]However, evolutionary models suggest that Wolf 359 is a relatively young star with an age of less than a billion years.[28]

Wolf 359's proper motion is 4.696arcsecondsper year, and moving away from the Sun at a velocity of ~19 km/s.[6][48]When translated into thegalactic coordinate system,the motion corresponds to aspace velocityof(U, V, W)=(−26, −44, −18) km/s.[49]This space velocity implies that Wolf 359 belongs to the population ofold-disk stars.It follows an orbit through theMilky Waythat will bring it as close as 20.5 kly (6.3 kpc) and as distant as 28 kly (8.6 kpc) from theGalactic Center.The predicted galactic orbit has aneccentricityof 0.156, and the star can travel as far as 444 light-years (136 pc) away from thegalactic plane.[50]The closest stellar neighbor to Wolf 359 is the red dwarfRoss 128,at 3.79ly(1.16pc).[51]Approximately 13,850 years before the present day, Wolf 359 attained its minimal separation of about 7.35 ly (2.25 pc) from the Sun, and has been receding away ever since.[52]

Search for planets

[edit]

Radial velocitymeasurements of the star in 2011 using the Near Infrared Spectrometer (NIRSPEC) instrument at theKeck IIobservatory did not reveal any variations that might otherwise indicate the presence of an orbiting companion. This instrumentation is sensitive enough to detect thegravitational perturbationsof massive, short period companions with the mass ofNeptuneor greater.[53]

In June 2019, an international team of astronomers led byMikko Tuomifrom theUniversity of Hertfordshire,UK, submitted apreprintwith the results of the first reported detection of two candidate exoplanets orbiting Wolf 359 using theradial velocity methodfrom observations withHARPSin Chile andHIRESin Hawaii.[54]If these planets were confirmed, the setup of the system would be similar to but more extreme than that of the nearby red dwarfProxima Centauri,with both having a close-in low-mass planet and a farther out higher-mass planet. The theorized and later ruled-out inner planet, Wolf 359 c, would receive per unit area about forty times as much radiative energy as compared to Earth, making it unlikely to be a habitable planet. The as yet unconfimed Wolf 359 b, in contrast, is classified as a cool super-Neptune,receiving roughly a third to a quarter of the energy per unit area as Neptune does from the Sun.[54]

Further observations from theCARMENES surveyhave found that the radial velocity signal corresponding to the inner planet candidate Wolf 359 c is a false positive, resulting from the rotation of the star rather than a planetary companion.[13][55]A 2023 follow-up study using MAROON-X, CARMENES, HARPS, and HIRES radial velocity data as well as imaging data was unable to either confirm or refute the presence of Wolf 359 b. The same study ruled out the existence of anybrown dwarfsor massive gas giant companions within 10AUof the star, planets more than half the mass of Jupiter within 1 AU, and planets more massive thanUranuswithin 0.1 AU.[14]

The Wolf 359 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b(unconfirmed) ≥43.9+29.5
−23.9M🜨 		1.845+0.289
−0.258 		2,938±436 0.04+0.27
−0.04 		— —

See also

[edit]

References

[edit]
  1. ^abcdVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  2. ^abcLandolt, Arlo U. (May 2009). "UBVRI photometric standard stars around the celestial equator: Updates and Additions".The Astronomical Journal.137(5): 4186–4269.arXiv:0904.0638.Bibcode:2009AJ....137.4186L.doi:10.1088/0004-6256/137/5/4186.S2CID118627330.See table II.
  3. ^abHenry, Todd J.; et al. (October 1994)."The solar neighborhood, 1: Standard spectral types (K5-M8) for northern dwarfs within eight parsecs".The Astronomical Journal.108(4): 1437–1444.Bibcode:1994AJ....108.1437H.doi:10.1086/117167.
  4. ^abCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)".CDS/ADC Collection of Electronic Catalogues.2246:II/246.Bibcode:2003yCat.2246....0C.
  5. ^abGershberg, R. E.; et al. (1983). "Characteristics of activity energetics of the UV Cet-type flare stars".Astrophysics and Space Science.95(2): 235–253.Bibcode:1983Ap&SS..95..235G.doi:10.1007/BF00653631.S2CID122101052.
  6. ^abcMohanty, Subhanjoy; et al. (2003). "Rotation and activity in mid-M to L field dwarfs".The Astrophysical Journal.583(1): 451–472.arXiv:astro-ph/0201455.Bibcode:2003ApJ...583..451M.doi:10.1086/345097.S2CID119463177.
  7. ^Houdebine, Éric R.; Mullan, D. J.; Doyle, J. G.; de la Vieuville, Geoffroy; Butler, C. J.; Paletou, F. (2019)."The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs".The Astronomical Journal.158(2): 56.arXiv:1905.07921.Bibcode:2019AJ....158...56H.doi:10.3847/1538-3881/ab23fe.S2CID159041104.
  8. ^abcdefPineda, J. Sebastian; Youngblood, Allison; France, Kevin (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.S2CID235435757.40.
  9. ^abCantrell, Justin R.; et al. (October 2013). "The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors".The Astronomical Journal.146(4): 99.arXiv:1307.7038.Bibcode:2013AJ....146...99C.doi:10.1088/0004-6256/146/4/99.S2CID44208180.
  10. ^Fuhrmeister, B.; et al. (September 2005). "PHOENIX model chromospheres of mid- to late-type M dwarfs".Astronomy and Astrophysics.439(3): 1137–1148.arXiv:astro-ph/0505375.Bibcode:2005A&A...439.1137F.doi:10.1051/0004-6361:20042338.S2CID16499769.
  11. ^Mann, Andrew W.; et al. (May 2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius".The Astrophysical Journal.804(1): 38.arXiv:1501.01635.Bibcode:2015ApJ...804...64M.doi:10.1088/0004-637X/804/1/64.S2CID19269312.64.
  12. ^Díez Alonso, E.; Caballero, J. A.; Montes, D.; De Cos Juez, F. J.; Dreizler, S.; Dubois, F.; Jeffers, S. V.; Lalitha, S.; Naves, R.; Reiners, A.; Ribas, I.; Vanaverbeke, S.; Amado, P. J.; Béjar, V. J. S.; Cortés-Contreras, M.; Herrero, E.; Hidalgo, D.; Kürster, M.; Logie, L.; Quirrenbach, A.; Rau, S.; Seifert, W.; Schöfer, P.; Tal-Or, L. (2019). "CARMENES input catalogue of M dwarfs. IV. New rotation periods from photometric time series".Astronomy and Astrophysics.621:A126.arXiv:1810.03338.Bibcode:2019A&A...621A.126D.doi:10.1051/0004-6361/201833316.S2CID111386691.
  13. ^abLafarga, M.; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J.; Caballero, J. A.; Azzaro, M.; Béjar, V. J. S.; Cortés-Contreras, M.; Dreizler, S.; Hatzes, A. P.; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Montes, D.; Morales, J. C.; Oshagh, M.; Rodríguez-López, C.; Schöfer, P.; Schweitzer, A.; Zechmeister, M. (2021). "The CARMENES search for exoplanets around M dwarfs. Mapping stellar activity indicators across the M dwarf domain".Astronomy and Astrophysics.652:652.arXiv:2105.13467.Bibcode:2021A&A...652A..28L.doi:10.1051/0004-6361/202140605.S2CID235248016.
  14. ^abcBowens-Rubin, Rachel; Akana Murphy, Joseph M.; et al. (December 2023)."A Wolf 359 in sheep's clothing: Hunting for substellar companions in the fifth-closest system using combined high-contrast imaging and radial velocity analysis".The Astronomical Journal.166(6): 260.arXiv:2309.03402.Bibcode:2023AJ....166..260B.doi:10.3847/1538-3881/ad03e5.
  15. ^"V* CN Leo -- Flare Star".SIMBAD.Centre de Données astronomiques de Strasbourg.Retrieved2007-07-16.
  16. ^Weir, Andy (2022).Project Hail Mary.London: Penguin Books.ISBN978-1-5291-5746-8.
  17. ^abMcLean, Ian S.; et al. (October 2003). "The NIRSPEC brown dwarf spectroscopic survey. I. low-resolution near-infrared spectra".The Astrophysical Journal.596(1): 561–586.arXiv:astro-ph/0309257.Bibcode:2003ApJ...596..561M.doi:10.1086/377636.S2CID1939667.
  18. ^Wolf, M. (1919). "Katalog von 1053 staerker bewegten Fixsternen".Veroeffentlichungen der Badischen Sternwarte zu Heidelberg.7(10): 195–219, 206.Bibcode:1919VeHei...7..195W.
  19. ^Wolf, M. (July 1917). "Eigenbewegungssterne".Astronomische Nachrichten.204(20): 345–350.Bibcode:1917AN....204..345W.doi:10.1002/asna.19172042002.
  20. ^van Maanen, Adriaan (1928). "The photographic determination of stellar parallaxes with the 60- and 100-inch reflectors. Fifteenth Series".Contributions from the Mount Wilson Observatory.356:1–27.Bibcode:1928CMWCI.356....1V.
  21. ^van Biesbroeck, G. (August 1944). "The star of lowest known luminosity".The Astronomical Journal.51:61–62.Bibcode:1944AJ.....51...61V.doi:10.1086/105801.
  22. ^Kron, G. E.; et al. (1957). "Red and infrared magnitudes for 282 stars with known trigonometric parallaxes".Astronomical Journal.62:205–220.Bibcode:1957AJ.....62..205K.doi:10.1086/107521.
  23. ^Greenstein, Jesse L.; et al. (August 1970)."The faint end of the main sequence".Astrophysical Journal.161:519.Bibcode:1970ApJ...161..519G.doi:10.1086/150556.
  24. ^abReiners, Ansgar; et al. (2007). "Rapid magnetic flux variability on the flare star CN Leonis".Astronomy and Astrophysics.466(2): L13–L16.arXiv:astro-ph/0703172.Bibcode:2007A&A...466L..13R.doi:10.1051/0004-6361:20077095.S2CID17926213.
  25. ^Mukai, K.; et al. (August 1990)."Spectroscopy of faint, high latitude cataclysmic variable candidates".Monthly Notices of the Royal Astronomical Society.245(3): 385–391.Bibcode:1990MNRAS.245..385M.doi:10.1093/mnras/245.3.385.
  26. ^abRobinson, R. D.; et al. (1995). "A search for microflaring activity on dMe flare stars. I. Observations of the dM8e Star CN Leonis".Astrophysical Journal.451:795–805.Bibcode:1995ApJ...451..795R.doi:10.1086/176266.
  27. ^Jones, Lauren V. (2009).Stars and galaxies.Greenwood Guides to the Universe. ABC-CLIO. p. 50.ISBN978-0-313-34075-8.
  28. ^abcdePavlenko, Ya. V.; et al. (2006). "Spectral energy distribution for GJ406".Astronomy and Astrophysics.447(2): 709–717.arXiv:astro-ph/0510570.Bibcode:2006A&A...447..709P.doi:10.1051/0004-6361:20052979.S2CID119068354.
  29. ^Borgia, Michael P. (2006).Human vision and the night sky: hot [i.e. how] to improve your observing skills.Patrick Moore's practical astronomy series. Springer. p. 208.ISBN978-0-387-30776-3.
  30. ^Dantona, F.; et al. (September 15, 1985)."Evolution of very low mass stars and brown dwarfs. I - The minimum main-sequence mass and luminosity".Astrophysical Journal, Part 1.296:502–513.Bibcode:1985ApJ...296..502D.doi:10.1086/163470.
  31. ^Brown, T. M.;et al. (1998). "Accurate determination of the solar photospheric radius".Astrophysical Journal Letters.500(2): L195.arXiv:astro-ph/9803131.Bibcode:1998ApJ...500L.195B.doi:10.1086/311416.S2CID13875360.The radius of the Sun is 695.5 Mm. 16% of this is 111 Mm.
  32. ^Harvey, Samantha (March 4, 2010)."Jupiter: facts & figures".Solar System Exploration.NASA. Archived fromthe originalon December 15, 2003.Retrieved2010-05-28.
  33. ^McCook, G. P.; et al. (1995)."Fully convective M dwarfs".Villanova University. Archived fromthe originalon 2011-06-15.Retrieved2010-05-17.
  34. ^Adams, Fred C.; et al. (December 2004). "Red dwarfs and the end of the main sequence".Gravitational Collapse: From Massive Stars to Planets.Revista Mexicana de Astronomía y Astrofísica. pp. 46–49.Bibcode:2004RMxAC..22...46A.
  35. ^Schroeder, Daniel J.; et al. (2000)."A search for faint companions to nearby stars using the wide field planetary camera 2".The Astronomical Journal.119(2): 906–922.Bibcode:2000AJ....119..906S.doi:10.1086/301227.
  36. ^Gautier, T. N.; et al. (2007). "Far infrared properties of M dwarfs".The Astrophysical Journal.667(1): 527–.arXiv:0707.0464.Bibcode:2007ApJ...667..527G.doi:10.1086/520667.S2CID15732144.
  37. ^Lestrade, J.-F.; et al. (November 2009). "Search for cold debris disks around M-dwarfs. II".Astronomy and Astrophysics.506(3): 1455–1467.arXiv:0907.4782.Bibcode:2009A&A...506.1455L.doi:10.1051/0004-6361/200912306.S2CID17035185.
  38. ^Casagrande, Luca; et al. (September 2008)."M dwarfs: effective temperatures, radii and metallicities".Monthly Notices of the Royal Astronomical Society.389(2): 585–607.arXiv:0806.2471.Bibcode:2008MNRAS.389..585C.doi:10.1111/j.1365-2966.2008.13573.x.S2CID14353142.
  39. ^Verschuur, Gerrit L. (2003).Interstellar matters: essays on curiosity and astronomical discovery.Springer. pp. 253–254.ISBN978-0-387-40606-0.
  40. ^Pavlenko, Y. V.; et al. (December 2002). "Carbon monoxide bands in M dwarfs".Astronomy and Astrophysics.396(3): 967–975.arXiv:astro-ph/0210017.Bibcode:2002A&A...396..967P.doi:10.1051/0004-6361:20021454.S2CID8384149.
  41. ^Pesch, Peter (June 1972)."CaOH, a new triatomic molecule in stellar atmospheres".Astrophysical Journal.174:L155.Bibcode:1972ApJ...174L.155P.doi:10.1086/180970.
  42. ^Schmitt, J. H. M. M.; et al. (2001). "Ground-based observation of emission lines from the corona of a red-dwarf star".Nature.412(2): 508–510.Bibcode:2001Natur.412..508S.doi:10.1038/35087513.PMID11484044.S2CID4415051.
  43. ^Liefke, C.; Reiners, A.; Schmitt, J. H. M. M. (January 2007). "Magnetic field variations and a giant flare Multiwavelength observations of CN Leo".Memorie della Societa Astronomica Italiana.78:258–260.Bibcode:2007MmSAI..78..258L.
  44. ^Staff (January 7, 2007). "Calling Dr. Frankenstein!: interactive binaries show signs of induced hyperactivity". National Optical Astronomy Observatory.
  45. ^Schmitt, J. H. M. M.; et al. (September 1995)."The X-ray view of the low-mass stars in the solar neighborhood".Astrophysical Journal.450(9): 392–400.Bibcode:1995ApJ...450..392S.doi:10.1086/176149.
  46. ^Cwiok, M.; et al. (March 2006). "Search for optical counterparts of gamma ray burst".Acta Physica Polonica B.37(3): 919.Bibcode:2006AcPPB..37..919C.
  47. ^Röser, Siegfried (2008).Reviews in modern astronomy, cosmic matter.Wiley-VCH. pp. 49–50, 57.ISBN978-3-527-40820-7.
  48. ^Staff (June 8, 2007)."List of the nearest 100 stellar systems".Research Consortium on Nearby Stars.Retrieved2007-07-16.
  49. ^Gliese, W. (1969). "Catalogue of nearby stars".Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg.22:1.Bibcode:1969VeARI..22....1G.
  50. ^Allen, C.;et al. (1998). "The galactic orbits of nearby UV Ceti stars".Revista Mexicana de Astronomía y Astrofísica.34:37–46.Bibcode:1998RMxAA..34...37A.
  51. ^"Wolf 359".SolStation Company.Retrieved2006-08-10.
  52. ^"Annotations on V* CN Leo object".SIMBAD.Centre de Données astronomiques de Strasbourg.Retrieved2010-04-13.
  53. ^Rodler, F.; et al. (February 2012). "Search for radial velocity variations in eight M-dwarfs with NIRSPEC/Keck II".Astronomy & Astrophysics.538:A141.arXiv:1112.1382.Bibcode:2012A&A...538A.141R.doi:10.1051/0004-6361/201117577.S2CID56103966.
  54. ^abTuomi, M.; Jones, H. R. A.; Anglada-Escudé, G.; Butler, R. P.; Arriagada, P.; Vogt, S. S.; Burt, J.; Laughlin, G.; Holden, B.; Teske, J. K.; Shectman, S. A.; Crane, J. D.; Thompson, I.; Keiser, S.; Jenkins, J. S.; Berdiñas, Z.; Diaz, M.; Kiraga, M.; Barnes, J. R. (2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood".arXiv:1906.04644[astro-ph.EP].
  55. ^Ribas, I.; Reiners, A.; et al. (February 2023)."The CARMENES search for exoplanets around M dwarfs. Guaranteed time observations Data Release 1 (2016-2020)".Astronomy & Astrophysics.670.arXiv:2302.10528.Bibcode:2023A&A...670A.139R.doi:10.1051/0004-6361/202244879.
[edit]
Wikimedia Commons has media related toWolf 359.

Retrieved from "https://en.wikipedia.org/w/index.php?title=Wolf_359&oldid=1235401946"