Photometry of selected outer main belt asteroids

• Main Authors: Shevchenko, V, Mikhalchenko, O, Belskaya, I, Slyusarev, I, Chiorny, V, Krugly, Yu, Hromakina, T, Dovgopol, A, Kiselev, N, Rublevsky, A, Antonyuk, K, Novichonok, A, Kusakin, A, Reva, I, Inasaridze, R, Ayvazian, V, Kapanadze, G, Molotov, I, Oszkiewicz, D, Kwiatkowski, T
• Format: Journal Article
• Language: English
• Published: 20-05-2021
• Subjects: Physics - Earth and Planetary Astrophysics
• DOI: 10.48550/arxiv.2105.09763

We present new photometric observations for twelve asteroids ((122) Gerda,
(152) Atala, (260) Huberta, (665) Sabine, (692) Hippodamia, (723) Hammonia,
(745) Mauritia, (768) Struveana, (863) Benkoela, (1113) Katja, (1175) Margo,
(2057) Rosemary) from the outer part of the main belt aimed to obtain the
magnitude-phase curves and to verify geometric albedo and taxonomic class based
on their magnitude-phase behaviors. The measured magnitude-phase relations
confirm previously determined composition types of (260) Huberta (C-type),
(692) Hippodamia (S-type) and (1175) Margo (S-type). Asteroids (665) Sabine and
(768) Struveana previously classified as X-type show phase-curve behavior
typical for moderate-albedo asteroids and may belong to the M-type. The
phase-curve of (723) Hammonia is typical for the S-type which contradicts the
previously determined C-type. We confirmed the moderate-albedo of asteroids
(122) Gerda and (152) Atala, but their phase-curves are different from typical
for the S-type and may indicate more rare compositional types. Based on
magnitude-phase behaviors and V-R colors, (2057) Rosemary most probably belongs
to M-type, while asteroids (745) Mauritia and (1113) Katja belong to S-complex.
The phase curve of the A-type asteroid (863) Benkoela does not cover the
opposition effect range and further observations are needed to understand
typical features of the phase-curves of A-type asteroids in comparison with
other types. We have also determined lightcurve amplitudes of the observed
asteroids and obtained new or improved values of the rotation periods for most
of them.