HIGH-SPEED PHOTOMETRY OF THE DISINTEGRATING PLANETESIMALS AT WD1145+017: EVIDENCE FOR RAPID DYNAMICAL EVOLUTION

被引：67

作者：

Gaensicke, B. T. ^{[1
]}

Aungwerojwit, A. ^{[2
]}

Marsh, T. R. ^{[1
]}

Dhillon, V. S. ^{[3
,4
]}

Sahman, D. I. ^{[3
]}

Veras, Dimitri ^{[1
]}

Farihi, J. ^{[5
]}

Chote, P. ^{[1
]}

Ashley, R. ^{[1
]}

Arjyotha, S. ^{[6
]}

Rattanasoon, S. ^{[7
]}

Littlefair, S. P. ^{[3
]}

Pollacco, D. ^{[1
]}

Burleigh, M. R. ^{[8
]}

机构：

[1] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[2] Naresuan Univ, Dept Phys, Fac Sci, Phitsanulok 65000, Thailand

[3] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England

[4] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain

[5] UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England

[6] Chiang Rai Rajabhat Univ, Fac Sci & Technol, Program Phys, Chiang Rai 57100, Thailand

[7] Natl Astron Res Inst Thailand, 191 Siriphanich Bldg,Huay Kaew Rd, Chiang Mai 50200, Thailand

[8] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2016年 / 818卷 / 01期

基金：

英国科学技术设施理事会; 欧洲研究理事会;

关键词：

minor planets; asteroids:; general; planetary systems; stars: individual (WD 1145+017); PLANETARY DEBRIS DISCS; POLLUTED WHITE-DWARF; MINOR PLANET; ASTEROIDS; SYSTEMS; CONSTRAINTS; ACCRETION; FREQUENCY; BODIES; WATER;

D O I：

10.3847/2041-8205/818/1/L7

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We obtained high-speed photometry of the disintegrating planetesimals orbiting the white dwarf WD 1145+017, spanning a period of four weeks. The light curves show a dramatic evolution of the system since the first observations obtained about seven months ago. Multiple transit events are detected in every light curve, which have varying durations (similar or equal to 3-12 minutes) and depths (similar or equal to 10%-60%). The time-averaged extinction is similar or equal to 11%, much higher than at the time of the Kepler observations. The shortest-duration transits require that the occulting cloud of debris has a few times the size of the white dwarf, longer events are often resolved into the superposition of several individual transits. The transits evolve on timescales of days, both in shape and in depth, with most of them gradually appearing and disappearing over the course of the observing campaign. Several transits can be tracked across multiple nights, all of them recur on periods of similar or equal to 4.49 hr, indicating multiple planetary debris fragments on nearly identical orbits. Identifying the specific origin of these bodies within this planetary system, and the evolution leading to their current orbits remains a challenging problem.

引用

页数：6

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