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Photometry and spin rates of 4 NEAs recently observed by the Mexican Asteroid Photometry Campaign

Published online by Cambridge University Press:  03 March 2020

J. C. Saucedo ,
S. A. Ayala-Gómez ,
M. E. Contreras ,
S. A. R. Haro-Corzo ,
P. A. Loera-González ,
L. Olgun  and
P. A. Valdés-Sada
J. C. Saucedo
Affiliation:
Departamento de Investigación en Fsica, Universidad de Sonora Blvd. Rosales y Colosio, Ed. 3H, 83190Hermosillo, Sonora, México email: jsaucedo@cifus.uson.mx
S. A. Ayala-Gómez
Affiliation:
FCFM–Universidad Autónoma de Nuevo León
M. E. Contreras
Affiliation:
Departamento de Investigación en Fsica, Universidad de Sonora Blvd. Rosales y Colosio, Ed. 3H, 83190Hermosillo, Sonora, México email: jsaucedo@cifus.uson.mx
S. A. R. Haro-Corzo
Affiliation:
ENES–Universidad Nacional Autónoma de México
P. A. Loera-González
Affiliation:
Departamento de Investigación en Fsica, Universidad de Sonora Blvd. Rosales y Colosio, Ed. 3H, 83190Hermosillo, Sonora, México email: jsaucedo@cifus.uson.mx
L. Olgun
Affiliation:
Departamento de Investigación en Fsica, Universidad de Sonora Blvd. Rosales y Colosio, Ed. 3H, 83190Hermosillo, Sonora, México email: jsaucedo@cifus.uson.mx
P. A. Valdés-Sada
Affiliation:
DFM–Universidad de Monterrey
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Abstract

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We present photometric observations of (4055) Magellan, (143404) 2003 BD44, 2014 JO25 and (3122) Florence, four potentially hazardous Near Earth Asteroids (NEAs). The data were taken near their approaches to Earth by 3 observatories participating in the Mexican Asteroid Photometry Campaign (CMFA). The results obtained: light curves, spin rates, amplitudes and errors, are in general agreement with those obtained by others. During the day of a NEAs maximum approach to our planet, its light curve may present significant changes. In the spin rate, however, only minute changes are observed. 2014 JO25 is briefly discussed in this regard.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium A30: Astronomy in Focus XXX , August 2018 , pp. 31 - 34
Copyright
© International Astronomical Union 2020

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