Today we want to talk about 1194 Aletta, a topic that has sparked interest and debate in recent times. 1194 Aletta is an issue that affects people of all ages and backgrounds, and its relevance has been increasing in recent years. In this article, we will explore different aspects of 1194 Aletta, from its causes and consequences to possible solutions and approaches to address it. 1194 Aletta is an issue that concerns us all, and it is important to understand it and consider its implications in our current society. Join us on this tour of 1194 Aletta and discover more about this exciting topic.
1194 Aletta, provisional designation 1931 JG, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 55 kilometers in diameter. It was discovered on 13 May 1931, by South African astronomer Cyril Jackson at Johannesburg Observatory in South Africa.[13] It was later named after the discoverer's wife Aletta Jackson.[2]
Classification and orbit
Aletta is a dark C-type asteroid and orbits the Sun at a distance of 2.6–3.2 AU once every 4 years and 12 months (1,816 days). Its orbit has an eccentricity of 0.09 and an inclination of 11° with respect to the ecliptic.[1] The body's observation arc begins at Johannesburg, one week after its official discovery observation. No precoveries were taken and no prior identifications were made.[13]
Physical characteristics
Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Aletta measures between 41.358 and 55.39 kilometers in diameter, and its surface has an albedo between 0.03 and 0.87.[4][5][6][7][8] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0333 and a diameter of 55.23 kilometers based on an absolute magnitude of 10.6.[3]
Rotation period
In November 2007, American astronomer James W. Brinsfield obtained the first ever lightcurve of Aletta with period of 19.7 hours and a brightness variation of 0.32 magnitude at Via Capote Observatory (U=2).[9] Two more lightcurves were obtained by Australian astronomer Julian Oey at Leura/Kingsgrove Observatory in March 2010, and by the Survey conducted at the Palomar Transient Factory, California, in October 2012. Lightcurve analysis gave a concurring rotation period of 20.39 and 20.3903 hours with an amplitude of 0.28 and 0.27 magnitude, respectively (U=2+/2).[10][11]
^ abcdUsui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)