LARGE SUPER-FAST ROTATOR HUNTING USING the INTERMEDIATE PALOMAR TRANSIENT FACTORY

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/102063

Title:	LARGE SUPER-FAST ROTATOR HUNTING USING the INTERMEDIATE PALOMAR TRANSIENT FACTORY
Authors:	章展誥;Chang, Chan-Kao;Lin, Hsing-Wen;Ip, Wing-Huen;Prince, Thomas A.;Kulkarni, Shrinivas R.;Levitan, David;Laher, Russ;Surace, Jason
Contributors:	理學院天文研究所
Keywords:	ASTEROIDS;ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;DETECTION;DIAGRAMS;EFFICIENCY;minor planets, asteroids: general;OVERBURDEN;PLANETS;ROTATION;SPIN;surveys;TRANSIENTS;VISIBLE RADIATION
Date:	2016-12-01
Issue Date:	2026-04-21 14:58:48 (UTC+8)
Publisher:	IOP Publishing Ltd.;United States: The American Astronomical Society
Abstract:	摘要： ABSTRACT In order to look for large super-fast rotators, in late 2014 and early 2015, five dedicated surveys covering ∼188 deg2 in the ecliptic plane have been carried out in the R-band, with ∼10 minute cadence using the intermediate Palomar Transient Factory. Among 1029 reliable rotation periods obtained from the surveys, we discovered 1 new large super-fast rotator, (40511) 1999 RE88, and 18 other candidates. (40511) 1999 RE88 is an S-type inner main-belt asteroid with a diameter of D = 1.9 ± 0.3 km, a rotation period of P = 1.96 ± 0.01 hr, and a light curve amplitude of Δm ∼ 1.0 mag. To maintain such fast rotation, an internal cohesive strength of ∼780 Pa is required. Combining all known large super-fast rotators, their cohesive strengths all fall in the range of 100-1000 Pa of lunar regolith. However, the number of large super-fast rotators seems to be far less than the whole asteroid population. This might indicate a peculiar asteroid group for them. Although the detection efficiency for a long rotation period is greatly reduced due to our two-day observation time span, the spin-rate distributions of this work show consistent results with Chang et al. (2015), after considering the possible observational bias in our surveys. It shows a number decrease with an increase of spin rate for asteroids with a diameter of 3 ⩽ D ⩽ 15 km, and a number drop at a spin rate of f = 5 rev day−1 for asteroids with D ⩽ 3 km. 其他題名： APJS 其他題名： Astrophys. J. Suppl 出版者： United States: The American Astronomical Society 出版日期： 2016-12-01 出處： The Astrophysical Journal Supplement Series, 2016-12, Vol.227 (2), p.20- 資源來源： Institute of Physics Journals 版權： 2016. The American Astronomical Society. All rights reserved. 識別號： ISSN: 0067-0049 識別號： ISSN: 1538-4365 識別號： EISSN: 1538-4365 識別號： DOI: 10.3847/0067-0049/227/2/20
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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