Brightness variation distributions among main belt asteroids from sparse light-curve sampling with Pan-STARRS 1

被引：18

作者：

McNeill, A. ^{[1
]}

Fitzsimmons, A. ^{[1
]}

Jedicke, R. ^{[2
]}

Wainscoat, R. ^{[2
]}

Denneau, L. ^{[2
]}

Veres, P. ^{[2
,3
]}

Magnier, E. ^{[2
]}

Chambers, K. C. ^{[2
]}

Kaiser, N. ^{[2
]}

Waters, C. ^{[2
]}

机构：

[1] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland

[2] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA

[3] Comenius Univ, Dept Astron Phys Earth & Meteorol, Bratislava 94248, Slovakia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 459卷 / 03期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

methods: statistical; minor planets; asteroids:; general; 25143; ITOKAWA; SPIN-STATE; YORP; EVOLUTION; ROTATION; YARKOVSKY;

D O I：

10.1093/mnras/stw847

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The rotational state of asteroids is controlled by various physical mechanisms including collisions, internal damping and the Yarkovsky-O'Keefe-Radzievskii-Paddack effect. We have analysed the changes in magnitude between consecutive detections of similar to 60 000 asteroids measured by the Panoramic Survey Telescope and Rapid Response System (PanSTARRS) 1 survey during its first 18 months of operations. We have attempted to explain the derived brightness changes physically and through the application of a simple model. We have found a tendency towards smaller magnitude variations with decreasing diameter for objects of 1 < D < 8 km. Assuming the shape distribution of objects in this size range to be independent of size and composition our model suggests a population with average axial ratios 1 : 0.85 +/- 0.13 : 0.71 +/- 0.13, with larger objects more likely to have spin axes perpendicular to the orbital plane.

引用

页码：2964 / 2972

页数：9

共 46 条

[1] Opposition effect of asteroids [J].