In October 2005, a rotational lightcurve of Erna was obtained from photometric observations by French and Italian astronomers Raymond Poncy (177), Roberto Crippa (A12), Federico Manzini and Silvano Casulli. Lightcurve analysis gave a well-defined rotation period of 8.7893 hours with a brightness variation of 0.35 magnitude (U=3).[12] Another lightcurve from the Palomar Transient Factory in November 2010 gave a similar period of 8.790 hours with an amplitude of 0.35 magnitude (U=2).[13]
Spin axis
In 2013, an international study modeled a lightcurve from various data sources including the Uppsala Asteroid Photometric Catalogue and the Palomar Transient Factory survey. The modeling gave a concurring period of 8.79079 hours and determined two spin axis in ecliptic coordinates (λ, β) of: (357.0°, −49.0°) and (161.0°, −60.0°).[14]
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, Erna measures between 41.52 and 49.19 kilometers in diameter and its surface has an albedo between 0.0524 and 0.060.[7][8][9][10][11][15]
The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0524 and a diameter of 49.19 kilometers based on an absolute magnitude of 10.36.[5][11]
Naming
This minor planet was likely named after Erna Bidschof, the granddaughter of Austrian astronomer Johann Palisa, who was one of the most prolific discoverer of minor planets at the time. Erna is the daughter of the astronomer Friedrich Bidschof (1864–1915) and his wife Helene (née Palisa).[4]
^ abcdeMasiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. S2CID46350317.
^ abcWaszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. S2CID8342929.
^ abHanus, J.; Durech, J.; Broz, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: 16. arXiv:1301.6943. Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. S2CID118627434.