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Assigned ID: 469
----- Attempting Submission 1 (Fri Apr 07 10:15:43 GMT 2017) -----
HST Phase I Proposal 469 (WD1145_Cycle25.apt) successfully submitted.
Receipt: # 469-1
----- Attempting Submission 2 (Fri Apr 07 11:27:37 GMT 2017) -----
HST Phase I Proposal 469 (WD1145_Cycle25.apt) successfully submitted.
Receipt: # 469-2
0
----- Attempting Submission 1 (Sat Jul 08 02:12:42 GMT 2017) -----
----- Attempting Submission 2 (Tue May 08 01:16:50 GMT 2018) -----
----- Attempting Submission 3 (Sat Jul 14 02:33:32 GMT 2018) -----
----- Attempting Submission 4 (Fri Aug 09 20:53:41 GMT 2019) -----
----- Attempting Submission 5 (Sat Oct 19 03:31:21 GMT 2019) -----
----- Attempting Submission 6 (Tue May 12 17:48:10 GMT 2020) -----
Actively Disintegrating Astroids around a White Dwarf
Recent studies show that planetary systems can be widespread around white dwarfs. It has been proposed that planetary systems are responsible for the pollution observed in a white dwarf's atmosphere and the excess infrared radiation. This scenario is greatly strengthened by the recent discovery of actively disintegrating bodies orbiting around the white dwarf WD 1145+017. In addition, this system has a heavily polluted atmosphere, a dust disk, and circumstellar gas. Our team has been monitoring this system since its discovery and our recent COS data have revealed many new surprises. We propose to continue studying this system for the next two cycles and further constrain the evolution of the disintegrating bodies: what are the main mechanisms responsible for its destruction? How is circumstellar gas produced and maintained?
We aim to understand WD 1145+017 system, which has a heavily polluted atmosphere, a dust disk, at least two circumstellar gas components as well as multiple transiting objects. COS observations can uniquely monitor the pollution, circumstellar gas, and transiting objects simultaneously. Here, we propose to obtain a full FUV spectrum of this rapidly evolving object. Specifically, our goal is threefold: (i) Understand the evolution of circumstellar gas; (ii) Study the change of UV light curve; (iii) Explore new spectral features. To have a continuous coverage from 1130 to 1800 Anstrom, we request four set-ups, two with G130M (central wavelength of 1291 Angstrom and 1327 Angstrom), and two with G160M (central wavelength of 1577 Anstrom and 1623 Angstrom).
Planets and Planet Formation
Stellar Physics
6
false
false
true
false
false
false
false
SUPPORTED
STAR
DB
NO
J2000
J2000
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/FUV
Spectroscopic
No
No
G130M
1327
COS/FUV
Spectroscopic
No
No
G160M
1623
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