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Lalande 21185 (also known as BD+36 2147, Gliese 411, and HD 95735[3]) is a star in the south of Ursa Major. It is the apparent brightest red dwarf in the northern hemisphere.[nb 2][10][11] Despite this, and being relatively close by, it is (as are all red dwarfs) very dim, being only magnitude 7.5 in visible light and thus too faint to be seen with the unaided eye. The star is visible through a small telescope or binoculars.[12]

Lalande 21185
The red circle shows the approximate location of Lalande 21185 in Ursa Major
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
Right ascension 11h 03m 20.19400s[1]
Declination +35° 58′ 11.5682″[1]
Apparent magnitude (V) 7.520[2]
Characteristics
Spectral type M2V[3]
Apparent magnitude (B) 8.960 ± 0.007[2]
Apparent magnitude (V) 7.520 ± 0.009[2]
Apparent magnitude (R) ~6.6[3]
Apparent magnitude (I) ~5.8[3]
Apparent magnitude (J) 4.203 ±0.242[3]
Apparent magnitude (H) 3.640 ±0.202[3]
Apparent magnitude (K) 3.254 ±0.306[3]
U−B color index +1.074[2]
B−V color index +1.444[2]
Variable type BY[4]
Astrometry
Radial velocity (Rv)−85.6 ± 1.0[5] km/s
Proper motion (μ) RA: −580.27[1] mas/yr
Dec.: −4765.85[1] mas/yr
Parallax (π)392.7529 ± 0.0321 mas[6]
Distance8.3044 ± 0.0007 ly
(2.5461 ± 0.0002 pc)
Absolute magnitude (MV)10.48[7]
Details
Mass0.389±0.008[8] M☉
Radius0.392±0.004[8] R☉
Luminosity (bolometric)0.0195±0.0013[9] L☉
Luminosity (visual, LV)0.0055[nb 1] L☉
Surface gravity (log g)4.87±0.07[9] cgs
Temperature3,547±18[8] K
Metallicity [Fe/H]−0.09±0.16[9] dex
Rotation56.15±0.27 d[9]
Age5–10[citation needed] Gyr
Other designations
NSV 18593, BD+36 2147, GJ 411, HD 95735, HIP 54035, SAO 62377, G 119-052, LFT 756, LHS 37, LTT 12960, NLTT 26105, PLX 2576, IRAS 11005+3615, 2MASS J11032023+3558117, J11032027+3558203, MCC 594[3]
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata

At approximately 8.31 light-years (2.55 parsecs)[1] away it is one of the nearest stars to the Solar System; only the Alpha Centauri system, Barnard's Star, and Wolf 359 and the brown dwarfs Luhman 16 and WISE 0855−0714 are known to be closer.[13] Because of its proximity it is a frequent subject for astronomical surveys and other research and thus is known by numerous other designations, most commonly Gliese 411 and HD 95735. In approximately 19,900 years it will be at its closest, about 4.65 ly (1.43 pc) from the Sun, just over half its present distance.[14][15]


History


Distances of the nearest stars from 20,000 years ago until 80,000 years in the future
Distances of the nearest stars from 20,000 years ago until 80,000 years in the future

The celestial coordinates of Lalande 21185 were first published in 1801 by French astronomer Jérôme Lalande of the Paris Observatory in the star catalog Histoire céleste française. The catalog sequence numbers for majority of the observed stars, including this one, were introduced in its 1847 edition by Francis Baily.[16][17] Today this star is one of just a few that are still commonly referred to by their Lalande catalog number.[18]

In May 1857, Friedrich Wilhelm Argelander discovered the high proper motion of the star. It was sometimes called "Argelander's second star".[19][20][21] (The "first Argelander's star" is Groombridge 1830, whose high proper motion was discovered by Argelander earlier—in 1842).

Friedrich August Theodor Winnecke is reported to have made the first measurement of the star's parallax of 0.511 arc seconds in 1857–58 and thus first identifying Lalande 21185 as the second-closest-known star to the Sun, after the Alpha Centauri system.[20] Since that time better measurements have placed the star further away, but it remained the second-closest-known star system until the astrophotographic discovery of two dim red dwarfs, Wolf 359 and Barnard's Star, in the early 20th century.[22]


Properties


Lalande 21185 is a typical type-M main-sequence star (red dwarf) with about 39% of the mass of the Sun[8] and is much cooler than the Sun at 3,550 K. It is intrinsically dim with an absolute magnitude of 10.48, emitting most of its energy in the infrared.[7] The proportion of elements other than hydrogen and helium is estimated based on the ratio of iron to hydrogen in the star when compared to the Sun. The logarithm of this ratio is −0.20, indicating that the proportion of iron is about 10−0.20, or 63% of the Sun. The surface gravity of this relatively compact star is approximately 65 times greater than the gravity at Earth's surface (log g = 4.8 cgs),[23] which is more than twice the surface gravity of our Sun.

An X-ray light curve for a flare on NSV 18593, adapted from Pye et al. (2015)[24]
An X-ray light curve for a flare on NSV 18593, adapted from Pye et al. (2015)[24]

Lalande 21185 is listed as a BY Draconis type variable star in the General Catalogue of Variable Stars. It is identified by the variable star designation NSV 18593.[4] Several star catalogs, including SIMBAD, also classify it as a flare star. This conclusion is not supported by the primary reference these catalogs all use. The observations made in this reference show that it is rather quiet in comparison to other stars of its variable type.[25]

Lalande 21185 emits X-rays, and X-ray flares have been observed.[26][24]

It is the brightest star between variable CO Ursae Maj and the comparably bright star HD 95129 to its west (specifically by south) and is a little closer to the latter.


Planetary system


Data published in 2017 from the HIRES system at the Keck Observatory on Mauna Kea supported the existence of a close-in planet with an orbital period of just 9.8693±0.0016 days, being at least 3.8 MEarth.[27]

Artist's impression of a planet transiting Lalande 21185
Artist's impression of a planet transiting Lalande 21185

Further radial velocity research with the SOPHIE échelle spectrograph and review of the original signal found that the 9.9 day period was undetectable, and instead proposed, using both datasets, that an exoplanet orbiting the star with a period of either 12.95 or 1.08 days, much more probably 12.95 as 1-day-period exoplanets seem to be rare in systems. This would give the planet a minimum mass of 2.99 Earth masses. It is too close to the star, and so therefore too hot, to be in the habitable zone, at all points within its eccentric orbit.[28] The proposed planet on 12-day orbit was confirmed by CARMENES [ja] (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Echelle Spectrographs) project in 2020.[9]

A second planet on a much further orbit was initially noticed by SOPHIE, but the baseline was not long enough to confirm the several-year-long signal. The signal was confirmed in 2021 to be a planet with mass at least 18.0+2.9
−2.6 M🜨,[29] a lower-bound estimate later revised to 14.2±1.8 M🜨.[30]

A third planet, Gliese 411 d, is suspected to orbit between Gliese 411 b and Gliese 411 c with a period of 215 days.[30]

The Lalande 21185 planetary system[30]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥2.64±0.19 M🜨 0.0788+0.00056
−0.00057		 12.9395+0.0013
−0.0012		 0.052+0.057
−0.037		 — —
d (unconfirmed) ≥4.1±0.6 M🜨 0.5141+0.0038
−0.0039		 215.62+0.76
−0.73		 0.15+0.16
−0.11		 — —
c ≥14.2±1.8 M🜨 2.845+0.077
−0.067		 2806+110
−94		 0.08+0.1
−0.06		 — —

The habitable zone for this star, defined as the locations where liquid water could be present on an Earth-like planet, is at a radius of 0.11–0.24 AU, where 1 AU is the average distance from the Earth to the Sun.[31] The planet b has an equilibrium temperature of 370.1+5.8
−6.8 K. Other known planets are outside HZ boundaries too, but undetected low-mass ones may be orbiting in this region of this system as well.[9]


Past claims of planets


Dutch astronomer Peter van de Kamp wrote in 1945 that Lalande 21185 possessed an "unseen companion" of 0.06 M☉ (about 60 MJ).[32] In 1951 van de Kamp and his student Sarah Lippincott claimed the astrometric detection of a planetary system using photographic plates taken with the 24-inch (610 mm) refractor telescope at Swarthmore College's Sproul Observatory.[33] In the summer of 1960, Sarah Lippincott altered the 1951 claim, to a planet of 0.01 M☉ (that is, 10 MJ), an 8-year orbital period, eccentricity of 0.3, a semi-major axis[nb 3] of 0.083 AU.[34] She used the original photographic plates and new plates taken with the same telescope.[35] Photographic plates from this observatory, taken at the same time, were used by Van de Kamp for his erroneous claim of a planetary system for Barnard's Star. The plates made with the Sproul 24-inch refractor and used for these and other studies were in 1973 shown to be flawed;[36] as they were the next year with astrometric measurements made by George Gatewood of the Allegheny Observatory.[37]

In 1996 the same Gatewood prominently announced at an AAS meeting[38] and to the popular press[39] the discovery of multiple planets in this system, detected by astrometry. The initial report was based on a very delicate analysis of the star's position over the years, which suggested reflex orbital motion due to one or more companions. Gatewood claimed that such companions would usually appear more than 0.8 arcseconds from the red dwarf itself. Though, a paper by Gatewood published only a few years earlier[40] and later searches by others, using coronagraphs and multifilter techniques to reduce the scattered-light problems from the star, did not positively identify any such companions,[41] and so his claim remains unconfirmed and is now in doubt.

Before the 1980s, finding the radial velocity of red dwarfs was neither very accurate nor consistent, and so due to its apparent brightness and because it does not have a companion, this star, along with eleven other similar red dwarf stars, were chosen to have their radial velocity measured, to unprecedented high accuracy, by planet hunter Geoff Marcy.[42] No companion was detected around this star in this nor other contemporary surveys, and such early equipment would have picked up any planet exceeding 0.7 MJ in an extremely close orbit of 5 days or less; or exceeding 10 MJ at about Jupiter's orbital distance.[42]


See also



References


  1. van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
  2. Oja, T. (August 1985), "Photoelectric photometry of stars near the north Galactic pole. II", Astronomy and Astrophysics Supplement Series, 61: 331–339, Bibcode:1985A&AS...61..331O
  3. "HD 95735". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-05-29.
  4. "NSV 18593". General Catalogue of Variable Stars, Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2009-09-09.
  5. Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511
  6. 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.
  7. Johnson, H. M.; Wright, C. D. (November 1983), "Predicted infrared brightness of stars within 25 parsecs of the Sun", Astrophysical Journal Supplement Series, 53: 643–711, Bibcode:1983ApJS...53..643J, doi:10.1086/190905
  8. 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. 40.
  9. Stock, S.; et al. (2020), "The CARMENES search for exoplanets around M dwarfs Three temperate-to-warm super-Earths", Astronomy & Astrophysics, A112: 643, arXiv:2010.00474, Bibcode:2020A&A...643A.112S, doi:10.1051/0004-6361/202038820, S2CID 222090233
  10. Dickinson, David (2015-12-23). "14 Red Dwarf Stars to View with Backyard Telescopes". Universe Today. Retrieved 2016-12-04.
  11. Croswell, Ken (July 2002). "The Brightest Red Dwarf". KenCroswell.com. Retrieved 2016-12-04.
  12. Sherrod, P. Clay; Koed, Thomas L. (2003), A Complete Manual of Amateur Astronomy: Tools and Techniques for Astronomical Observations, Astronomy Series, Courier Dover Publications, p. 9, ISBN 978-0486428208
  13. "The 100 nearest star systems". Research Consortium On Nearby Stars. January 1, 2009. Retrieved 2009-09-09.
  14. García-Sánchez, J.; et al. (2001), "Stellar encounters with the solar system" (PDF), Astronomy and Astrophysics, 379 (2): 634–659, Bibcode:2001A&A...379..634G, doi:10.1051/0004-6361:20011330
  15. "Annotations on HD 95735 object". Centre de données astronomiques de Strasbourg. Retrieved 2010-04-14.
  16. Baily, Francis; Lalande, Joseph Jérôme Le Français de (1847). "Catalogue of those stars in the Histoire céleste française of Jérôme Delalande, for which tables of reduction to the epoch 1800 habe been published by Prof. Schumacher". London (1847). Bibcode:1847cshc.book.....B. Google Books id: oc0-AAAAcAAJ.
  17. Baily, F. (1847). "A catalogue of those stars in the "Histoire céleste française" of J. De Lalande for which tables of reduction to the session define format EPOCH1 = 1800 have been published by Professor Schumacher". British Ass. Adv. Sci. 1847. Bibcode:1950Lalan1847....0B.
  18. Joseph-Jérôme de Lalande Archived July 21, 2009, at the Wayback Machine
  19. Lynn, W. T. (1872). "On the Parallax and Proper Motion of Lalande 21185". Monthly Notices of the Royal Astronomical Society. 33: 52–54. Bibcode:1872MNRAS..33...52L. doi:10.1093/mnras/33.1.52.
  20. Winnecke, A. (1858). "Über die Parallaxe des zweiten Argelander'schen Sterns, von Herrn Prof. Winnecke". Astronomische Nachrichten. 48 (1147): 289–292. Bibcode:1858AN.....48..289W. doi:10.1002/asna.18580481903.
  21. Winnecke, Friedrich August Theodor (1872). "Bestimmung der parallaxe des zweiten Argelander-'schen sternes aus messungen AM heliometer der sternwarte zu Bonn in den jahren 1857–1858". Leipzig, W. Engelmann. Astronomische Gesellschaft, Leipzig. Publication11. Leipzig. Bibcode:1872bpza.book.....W. hdl:2027/nnc1.cu50717758.
  22. Russell, H. N. (June 1905). "The parallax of Lalande 21185 and γ Virginis from photographs taken at the Cambridge Observatory". Monthly Notices of the Royal Astronomical Society. 65 (8): 787–800. Bibcode:1905MNRAS..65..787R. doi:10.1093/mnras/65.8.787.
  23. Cayrel de Strobel, G.; et al., "A catalogue of Fe/H determinations", Astronomy and Astrophysics Supplement Series (1991 ed.), 95 (2): 273–336, Bibcode:1992A&AS...95..273C, ISSN 0365-0138
  24. Pye, J. P.; Rosen, S.; Fyfe, D.; Schröder, A. C. (September 2015). "A survey of stellar X-ray flares from the XMM-Newton serendipitous source catalogue: HIPPARCOS -Tycho cool stars" (PDF). Astronomy & Astrophysics. 581: A28. doi:10.1051/0004-6361/201526217. Retrieved 30 June 2022.
  25. Bopp, B. W.; Noah, P. V.; Klimke, A.; Africano, J. (October 1, 1981). "Discovery and observation of BY Draconis variables". Astrophysical Journal. 249 (1): 210–217. Bibcode:1981ApJ...249..210B. doi:10.1086/159277.
  26. Schmitt JHMM; Fleming TA; Giampapa MS (September 1995). "The X-Ray View of the Low-Mass Stars in the Solar Neighborhood". Astrophys. J. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi:10.1086/176149.
  27. Butler, R. Paul; Vogt, Steven S.; et al. (12 February 2017). "The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey". The Astronomical Journal. 153 (5): 208. arXiv:1702.03571. Bibcode:2017AJ....153..208B. doi:10.3847/1538-3881/aa66ca. S2CID 14954371.
  28. Díaz, Rodrigo F.; Delfosse, Xavier; Hobson, Melissa J.; Boisse, Isabelle; Astudillo-Defru, Nicola; Bonfils, Xavier; Henry, Gregory W.; Arnold, Luc; Bouchy, François; Bourrier, Vincent; Brugger, Bastien; Dalal, Shweta; Deleuil, Magali; Demangeon, Olivier D. S.; Dolon, François; Dumusque, Xavier; Forveille, Thierry; Hara, Nathan C.; Hébrard, Guillaume; Kiefer, Flavien; Lopez, Théo; Mignon, Lucile; Moreau, François; Mousis, Olivier; Moutou, Claire; Pepe, Francesco; Perruchot, Sandrine; Richaud, Yoann; Santerne, Alexandre; Santos, Nuno C.; Sottile, Rico; Stalport, Manu; Ségransan, Damien; Udry, Stéphane; Unger, Nicolas; Wilson, Paul A. (15 February 2019). "The SOPHIE search for northern extrasolar planets. XIV. A temperate ($T_\mathrm{eq}\sim 300$ K) super-earth around the nearby star Gliese 411". Astronomy & Astrophysics. A17: 625. arXiv:1902.06004. doi:10.1051/0004-6361/201935019. S2CID 85529763.
  29. Rosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard T.; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah C.; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T. (1 July 2021). "The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades" (PDF). The Astrophysical Journal Supplement Series. 255 (1): 8. arXiv:2105.11583. Bibcode:2021ApJS..255....8R. doi:10.3847/1538-4365/abe23c. S2CID 235186973.
  30. Hurt, Spencer A.; Fulton, Benjamin; Isaacson, Howard; Rosenthal, Lee J.; Howard, Andrew W.; Weiss, Lauren M.; Petigura, Erik A. (2021), "Confirmation of the Long-Period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate", The Astronomical Journal, 163 (5): 218, arXiv:2107.09087, Bibcode:2022AJ....163..218H, doi:10.3847/1538-3881/ac5c47, S2CID 236134034
  31. Cantrell, 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, S2CID 44208180
  32. van de Kamp, Peter (February 1945). "Stars Nearer than Five Parsecs". Publications of the Astronomical Society of the Pacific. 57 (334): 34–41 (34, 36, 39). Bibcode:1945PASP...57...34V. doi:10.1086/125679.
  33. van de Kamp, P.; Lippincott, S. L. (April 1951). "Astrometric study of Lalande 21185". The Astronomical Journal. 56: 49–50. Bibcode:1951AJ.....56...49V. doi:10.1086/106503.
  34. Lippincott, Sarah Lee (September 1960). "Astrometric analysis of Lalande 21185". Astronomical Journal. 65 (7): 445–448. Bibcode:1960AJ.....65..445L. doi:10.1086/108285.
  35. Lippincott, Sarah Lee (August 1960). "The Unseen Companion of the Fourth Nearest Star, Lalande 21185". The Astronomical Journal. 65: 350. Bibcode:1960AJ.....65..349L. doi:10.1086/108260.
  36. John L. Hershey (June 1973). "Astrometric analysis of the field of AC +65 6955 from plates taken with the Sproul 24-inch refractor". Astronomical Journal. 78 (5): 421–425. Bibcode:1973AJ.....78..421H. doi:10.1086/111436.
  37. Gatewood, G. (January 1974). "An astrometric study of Lalande 21185". The Astronomical Journal. 79 (1): 52. Bibcode:1974AJ.....79...52G. doi:10.1086/111530.
  38. Gatewood, G. (May 1996). "Lalande 21185". Bulletin of the American Astronomical Society. 28: 885. Bibcode:1996AAS...188.4011G.
  39. John Wilford (1996-06-12). "Data Seem to Show a Solar System Nearly in the Neighborhood". The New York Times. p. 1. Retrieved 2009-05-29.
  40. Gatewood; Stein, John; De Jonge, Joost K.; Persinger, Timothy; Reiland, Thomas; Stephenson, Bruce (September 1992). "Multichannel astrometric photometer and photographic astrometric studies in the regions of Lalande 21185, BD 56°2966, and HR 4784". The Astronomical Journal. 104 (3): 1237–1247. Bibcode:1992AJ....104.1237G. doi:10.1086/116313.
  41. Henry; Baliunas, Sallie L.; Donahue, Robert A.; Fekel, Francis C.; Soon, Willie (March 1, 2000). "Photometric and Ca II H and K Spectroscopic Variations in Nearby Sun-like Stars with Planets. III" (PDF). The Astrophysical Journal. 531 (1): 415–437. Bibcode:2000ApJ...531..415H. doi:10.1086/308466.
  42. Marcy; Lindsay, Victoria; Wilson, Karen (June 1987). "Radial velocities of M dwarf stars". Publications of the Astronomical Society of the Pacific. 99: 490–496. Bibcode:1987PASP...99..490M. doi:10.1086/132010.

Notes


  1. From knowing the absolute visual magnitude of Lalande 21185, , and the absolute visual magnitude of the Sun, = , the visual luminosity of Lalande 21185 can therefore be calculated: = 0.005495 Lv⊙
  2. Only AX Microscopii and Lacaille 9352, in the southern hemisphere, are brighter
  3. which would be orbital radius if e was 0, that is, a circular orbit



На других языках

[de] Lalande 21185

Lalande 21185 ist ein Stern der Spektralklasse M1.5 V. Es handelt sich um einen Roten Zwerg mit schwacher Leuchtkraft von 1/40 der Sonne, geringer Masse von ca. 0,4 Sonnenmassen, und einer relativ kühlen Oberflächentemperatur von 3600 Kelvin. Die scheinbare Helligkeit im V-Band beträgt 7,5 mag und die absolute Helligkeit 10,5 mag. Der Winkeldurchmesser wurde mit dem PTI (Palomar Testbed Interferometer) gemessen zu 1,464±0,03 Millibogensekunden. Daraus ergibt sich ein Durchmesser von 0,40 Sonnendurchmessern oder 555.000 km. Der Stern befindet sich im Sternbild Großer Bär in 8,3 Lichtjahren Entfernung. Damit ist er der sechstnächste bekannte Stern zur Sonne.
- [en] Lalande 21185

[es] Lalande 21185

Lalande 21185 (GJ 411)[1] es el nombre de la quinta estrella más cercana a nuestro Sol después de Alfa Centauri, la estrella de Barnard, Luhman 16 y Wolf 359. A pesar de su cercanía, solo tiene magnitud aparente +7,47 y no es visible a simple vista, aunque sí con cualquier telescopio pequeño. Se la localiza en el rincón sureste de la constelación de la Osa Mayor, al noroeste de Alula Borealis (ν Ursae Majoris) y al noreste de Praecipua (46 Leonis Minoris). Fue descubierta por Joseph-Jérôme Lefrançais de Lalande, quien fuera director del Observatorio de París.

[ru] Лаланд 21185

Лаланд 21185 (англ. Lalande 21185) — звезда, расположенная в созвездии Большая Медведица. Является одной из самых близких к Солнцу звёзд (расстояние около 8,31 световых лет).


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