Changes

| rightascension =11^h 03^m 20.194^s<ref name=hipp>van Leeuwen, F. (2007). Validation of the new Hipparcos reduction. ''Astronomy & Astrophysics'', 474(2), pp.653-664. [https://arxiv.org/abs/0708.1752 arXiv:0708.1752]</ref> | declination =+35^o 35° 58' 11.555682"<ref name=hipp/>

| magnitude =Apparent Mag:7.47<ref>T., O. (1985). Photoelectric photometry of stars near the North Galactic Pole. II. ''Astronomy and Astrophysics Supplement Series'', 61, pp.331-339. [https://ui.adsabs.harvard.edu/#abs/1985A&AS...61..331O Astrophysics Data System]</ref><br/>Absolute Mag: 10.4844<ref>From definition of absolute magnitude, using apparent magnitude (+7.47) and distance (8.32 ly) given here.</ref>

| radvelocity =<nowiki>-85.0 ±00±0.9 km/s</nowiki><ref>Nidever, D., Marcy, G., Butler, R., Fischer, D. and Vogt, S. (2002). Radial Velocities for 889 Late‐Type Stars. ''The Astrophysical Journal Supplement Series'', 141(2), pp.503-522. [https://arxiv.org/abs/astro-ph/0112477 arXiv:astro-ph/0112477]</ref>| propmotion =RA: -580.46 ±0.95 mas/yr<ref name=hipp/><br/>Dec.: -4769.95 ±0.53 mas/yr<ref name=hipp/>| parallax =392.52±0.91 mas<ref name=hipp/>

'''Lalande 21185''' is the closest system to Sol after [[Proxima Centauri]], [[Alpha Centauri]], [[Barnard's Star]], and [[Wolf 359]]. Located in the [[constellation ]] of [[Ursa Major]], it is only 8.3 light years away, although due to its low apparent magnitude of 7.5, it’s invisible to the unaided eye.<ref>[http://www.solstation.com/stars/la21185.htm Lalande 21185]from solstation.com</ref>

The star is a [[red dwarf]] with a spectral luminously M2.1 Vne and only contains about 40% of the mass of our own star. Lalande 21195 is also 46% of our Sun’s diameter and is only six-tenths of a percent as bright.<ref>http://joy.chara.gsu.edu/RECONS/TOP100.posted.htm</ref> The star's [[metallicity]] is only 63% of that of our [[Sun]], based on the amount of [[iron]] present.<ref>httpCayrel de Strobel, G., Hauck, B., François, P., Thévenin, F., Friel, E., Mermilliod, M. and Borde, S. (1992). A catalogue of [Fe/H] determinations: 1991 edition. ''Astronomy and Astrophysics Supplement Series'', 95, pp.273-336. [https://adsbitui.adsabs.harvard.edu/cgi-bin#abs/nph-iarticle_query?bibcode=1992A%26AS...95..273CAstrophysics Data System]</ref>

Lalande 21185 is actually moving perpendicular to the galactic plane at a relative velocity of 47&nbsp;km/s. Based on this observation, the star likely is one of the "thick disk" stars of our galaxy, belong to the [[Milky Way|Milky Way's]] thick disk, which has an average thickness of 3,500 light years. Most stars that belong to this group are [[metallicity|metal-poor]] stars that move in an eccentric orbit relative to the galactic plane.

In 1996 an astronomical team reported detecting two possible planets orbiting Lalande 21185.<ref>http[https://ui.adsabs.harvard.edu/cgi-bin#abs/nph-bib_query?bibcode=1996AAS...188.4011G&db_key=AST&high=38ef9e6de224494Astrophysics Data System]</ref> The closer of the two is estimated to exist some 2.2 AUs from its parent star and is 90% of [[Jupiter|Jupiter’s]] mass. The further possible planet may exist at the distance of 11 AUs and may be 1.6 times Jupiter’s mass. At this time neither world has been independently confirmed.<ref>httpHenry, G., Baliunas, S., Donahue, R., Fekel, F. and Soon, W. (2000). Photometric and CaiiH and K Spectroscopic Variations in Nearby Sun‐like Stars with Planets. III. ''The Astrophysical Journal'', 531(1), pp.415-437. [https://ui.adsabs.harvard.edu/cgi-bin#abs/nph-bib_query?bibcode=2000ApJ...531..415H&db_key=AST&high=38e0b7728700472Astrophysics Data System]</ref>