A specific non-gravitational effect and spin-parameters of the asteroids

1Kazantsev, AM, 1Kazantseva, LV
1Astronomical Observatory of Taras Shevchenko National University of Kyiv, Kyiv, Ukraine
Kinemat. fiz. nebesnyh tel (Online) 2019, 35(4):60-70
https://doi.org/10.15407/kfnt2019.04.060
Start Page: Dynamics and Physics of Solar System Bodies
Language: Russian
Abstract: 

Search for additional arguments for the reality of a specific non-gravitational effect in the asteroid belt (NGE), obtained more than ten years ago, has been performed. This NGE causes a gradual increase in the semi-major axes of orbits of low-albedo asteroids compare to the semi-major axes of orbits of asteroids with larger albedos. Such specific action of the NGE is confirmed by albedo distributions on the semi-major axes for separate asteroid families. The change of the major semi-axes of the orbits of the asteroids of the main belt due to the NGE (da) comes to 10-6 AU per 10 years. The physical mechanism of action of the NGE is similar to the cometary one. Therefore, the sign of the da values should depend on the direction of the axial rotation of the asteroids, and their absolute value |da| — upon the spin period P. Such relationship between da and P will be in the case of the Yarkovsky effect, but the latter is 3-4 orders of magnitude weaker than this NGE. At present, there are very few asteroids with precisely defined spin directions. Therefore, to confirm the reality of the NGE, data on the spin periods of asteroids were used. More than 12 thousands main belt asteroids were selected from the MPC base, for which spin periods were determined. The numerical calculations of the evolution of the orbits of the selected asteroids are performed for the interval from 2005 to 2016 and the corresponding da values are determined. The |da|(Р) dependencies are constructed and analyzed. The form of |da|(Р) dependencies is consistent with the theoretical dependencies at a level above 2σ. For more accurate values of the spin periods, the significance of the |da|(Р) dependence increases, although the number of such bodies is more than twice less than the total. The obtained result can be considered one more confirmation of the reality of the NGE existence.

Keywords: asteroid, non-gravitational effect, spin period
References: 

1. Kazantsev A. M. (2002) A simple method for numerical calculations of the evolution of orbits of near-Earth asteroids. Solar System Res. 36, № 1. P. 43—49.
https://doi.org/10.1023/A:1014273527226

2. Kazantsev A. M. (2007) Possible effect of spatial separation of bright and dark asteroids. Kinemat. Phys. Celest. Bodies. 23(6). 258—264.
https://doi.org/10.3103/S0884591314050031

https://doi.org/10.3103/S0884591307060037

3. Kazantsev A. M., Kazantseva L. V. (2008) On the residuals in asteroid catalogs and a possible nongravitational effect. Kinemat. Phys. Celest. Bodies. 24(5). 248—252. https://doi.org/10.3103/S0884591308050048

4. Kazantsev A. M., Kazantseva L. V. (2014) Additional criteria for identifying the aste¬roid families and confirmation of the effect of spatial separation of family members according to their albedos. Kinemat. Phys. Celest. Bodies. 30(5). 255—260. https://doi.org/10.3103/S0884591314050031

5. Kazantsev A. M., Kazantseva L. V. (2017) A specific nongravitational effect in the asteroid belt. Solar System Res. 51(6). 527—534.
https://doi.org/10.1134/S0038094617060053

6. Golubov O., Kravets Y., Krugly Yu. N., Scheeres D. J. (2016) Physical models for the normal YORP and diurnal Yarkovsky effects. Mon. Notic. Roy. Astron. Soc. 458(4). 3977—3989.
https://doi.org/10.1093/mnras/stw540

7. Masiero J. R., Mainzer A. K., Grav T., Bauer J. M., Cutri R. M., Dailey J., Eisenhardt P. R. M., McMillan R. S., Spahr T. B., Skrutskie M. F., et al. (2011) Main belt asteroids with WISE/NEOWISE. I. Preliminary albedos and diameters. Astrophys. J. 741(2). 20.
https://doi.org/10.1088/0004-637X/741/2/68

8. Spitale J., Greenberg R. (2001) Numerical evaluation of the general Yarkovsky effect: Effects on semimajor axis. Icarus. 149, № 1. P. 222—234.
https://doi.org/10.1006/icar.2000.6477