мЮИДЕМШ МНБШЕ ГМЮВЕМХЪ ЛЮЯЯ ЙПСОМШУ ЮЯРЕПНХДНБ Х НАЫЕИ ЛЮЯЯШ ЦКЮБМНЦН ЮЯРЕПНХДМНЦН ОНЪЯЮ. дКЪ ВЮЯРХ НАЗЕЙРНБ СДЮЕРЯЪ ОНКСВХРЭ ОПЪЛШЕ ДХМЮЛХВЕЯЙХЕ НЖЕМЙХ ЛЮЯЯ ОН ЦПЮБХРЮЖХНММНЛС БГЮХЛНДЕИЯРБХЧ Я ДПСЦХЛХ РЕКЮЛХ. лЮЯЯШ ДПСЦХУ ЙПСОМШУ ЮЯРЕПНХДНБ НЖЕМХБЮЧРЯЪ ОН ХУ ДХЮЛЕРПЮЛ Х ОНКСВЕММШЛ ОКНРМНЯРЪЛ. нЖЕМЙЮ ЛЮЯЯШ НЯРЮБЬЕИЯЪ ВЮЯРХ ЛМНЦНВХЯКЕММШУ АНКЕЕ ЛЕКЙХУ ЮЯРЕПНХДНБ ОПНБНДХРЯЪ ОН ХУ ЯСЛЛЮПМНЛС ЦПЮБХРЮЖХНММНЛС БКХЪМХЧ МЮ ДПСЦХЕ РЕКЮ. пЮАНРЮ АШКЮ БШОНКМЕМЮ МЮ НЯМНБЕ МНБНИ БЕПЯХХ ОКЮМЕРМНИ РЕНПХХ EPM2013 Я ХЯОНКЭГНБЮМХЕЛ АНКЕЕ 792 РШЯЪВ ОНГХЖХНММШУ МЮАКЧДЕМХИ ОКЮМЕР Х ЙНЯЛХВЕЯЙХУ ЮООЮПЮРНБ (1913–2012 ЦЦ.). дКЪ АНКЕЕ РНВМНИ НЖЕМЙХ НАЫЕИ ЛЮЯЯШ МЕАНКЭЬХУ ЮЯРЕПНХДНБ ХУ ЯСЛЛЮПМНЕ ЦПЮБХРЮЖХНММНЕ БКХЪМХЕ ЛНДЕКХПСЕРЯЪ ДБСЛЕПМШЛ ЙНКЭЖНЛ Я ПЮГЛЕПЮЛХ, ЯННРБЕРЯРБСЧЫХЛХ МЮАКЧДЮЕЛНИ ЬХПХМЕ ЦКЮБМНЦН ОНЪЯЮ. щРН ОПХБЕКН Й ЯСЫЕЯРБЕММНЛС СЛЕМЭЬЕМХЧ НЬХАЙХ Б НОПЕДЕКЕМХХ ЛЮЯЯШ ОНЪЯЮ ЮЯРЕПНХДНБ. мЮИДЕММНЕ ГМЮВЕМХЕ НАЫЕИ ЛЮЯЯШ ЦКЮБМНЦН ОНЪЯЮ ЮЯРЕПНХДНБ ЯНЯРЮБКЪЕР (12.25 ± 0.19)·10^-10 ЛЮЯЯШ яНКМЖЮ.

An updated database of planet and spacecraft observations, as well as asteroid data, has been used to improve the asteroid (included main belt asteroid) masses and perturbations caused by them on the motion of Solar System bodies. The direct estimation of the dynamical mass was obtained for a part of asteroids from their gravitation impacts on other celestial bodies. The masses of other large asteroids were calculated from their diameters and estimated densities.
The mass of all the remaining small asteroids is estimated from the total gravitational influence caused by a two-dimensional ring with a constant mass distribution in the ecliptic plane.
The work is based on the new version of the EPM2013 ephemerides and more than 792 000 positional observations (mainly radar ones) of planets and spacecraft made from 1913 to 2012. It is our first experience with a two-dimensional asteroid ring with dimensions obtained from its observable width instead of one-dimensional rings which we considered in our previous versions of EPM ephemerides for modeling perturbations of small asteroids. As a result, the accuracy of the two-dimensional asteroid ring's mass has grown considerably; orbits of all planets are obviously improved, and a particularly important gain is that the formal uncertainties o f the planets' semi-major axes has been halved. The total mass of the main asteroid belt is found: M_belt = (12.25 ± 0.19) 10^-10 M_Sun or ≈ 2.5 M_Ceres.