Email this article Confirmation of the Sublimation Activity of the Primitive Main-Belt Asteroids 779 Nina, 704 Interamnia, and 145 Adeona, as well as its Probable Spectral Signs on 51 Nemausa and 65 Cybele
- Authors: Busarev V.V.1,2, Shcherbina M.P.1, Barabanov S.I.2, Irsmambetova T.R.1, Kokhirova G.I.3, Khamroev U.K.3, Khamitov I.M.4,5, Bikmaev I.F.5,6, Gumerov R.I.5,6, Irtuganov E.N.5,6, Mel’nikov S.S.5,6
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Affiliations:
- Sternberg Astronomical Institute, Moscow State University
- Institute of Astronomy (INASAN), Russian Academy of Sciences
- Institute of Astrophysics, Academy of Sciences of the Republic of Tajikistan
- TÜBİTAK National Observatory
- Kazan Federal University
- Academy of Sciences of the Republic of Tatarstan
- Issue: Vol 53, No 4 (2019)
- Pages: 261-277
- Section: Article
- URL: https://journal-vniispk.ru/0038-0946/article/view/171354
- DOI: https://doi.org/10.1134/S0038094619040014
- ID: 171354
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Abstract
This paper presents the results that confirm the sublimation activity at the perihelion of the primitive main-belt asteroids 779 Nina, 704 Interamnia, and 145 Adeona; this activity was first discovered in September 2012 (Busarev et al., 2015; Busarev et al., 2016). The new spectrophotometric and/or UBVRI photometric observations of Nina, Interamnia, and Adeona were carried out in 2016–2018 during a regular perihelion passage of these asteroids. Additionally, probable spectral signs of weak sublimation activity were discovered on another two primitive main-belt asteroids, 51 Nemausa and 65 Cybele. In this study, we discuss the conditions for the occurrence of a periodic and/or continuous sublimation process on main-belt asteroids with low-temperature mineralogy; in particular, the conditions that are associated with their formation close to the “snow line” or beyond. We also consider general evolution processes that are able sustain a sufficiently high concentration of water ice close to the surface of the bodies in question and, therefore, their continuous sublimation activity, or lead to the recurrence of extinct activity.
About the authors
V. V. Busarev
Sternberg Astronomical Institute, Moscow State University; Institute of Astronomy (INASAN), Russian Academy of Sciences
Author for correspondence.
Email: busarev@sai.msu.ru
Russian Federation, Moscow; Moscow
M. P. Shcherbina
Sternberg Astronomical Institute, Moscow State University
Email: busarev@sai.msu.ru
Russian Federation, Moscow
S. I. Barabanov
Institute of Astronomy (INASAN), Russian Academy of Sciences
Email: busarev@sai.msu.ru
Russian Federation, Moscow
T. R. Irsmambetova
Sternberg Astronomical Institute, Moscow State University
Email: busarev@sai.msu.ru
Russian Federation, Moscow
G. I. Kokhirova
Institute of Astrophysics, Academy of Sciences of the Republic of Tajikistan
Email: busarev@sai.msu.ru
Tajikistan, Dushanbe
U. Kh. Khamroev
Institute of Astrophysics, Academy of Sciences of the Republic of Tajikistan
Email: busarev@sai.msu.ru
Tajikistan, Dushanbe
I. M. Khamitov
TÜBİTAK National Observatory; Kazan Federal University
Email: busarev@sai.msu.ru
Turkey, Antalya; Kazan
I. F. Bikmaev
Kazan Federal University; Academy of Sciences of the Republic of Tatarstan
Email: busarev@sai.msu.ru
Russian Federation, Kazan; Kazan
R. I. Gumerov
Kazan Federal University; Academy of Sciences of the Republic of Tatarstan
Email: busarev@sai.msu.ru
Russian Federation, Kazan; Kazan
E. N. Irtuganov
Kazan Federal University; Academy of Sciences of the Republic of Tatarstan
Email: busarev@sai.msu.ru
Russian Federation, Kazan; Kazan
S. S. Mel’nikov
Kazan Federal University; Academy of Sciences of the Republic of Tatarstan
Email: busarev@sai.msu.ru
Russian Federation, Kazan; Kazan
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