Phase‐resolvedHubble Space Telescope/STIS Spectroscopy of the Exposed White Dwarf in the High‐Field Polar AR Ursae Majoris

2001 ◽  
Vol 555 (1) ◽  
pp. 380-392 ◽  
Author(s):  
Boris T. Gansicke ◽  
Gary D. Schmidt ◽  
Stefan Jordan ◽  
Paula Szkody
Keyword(s):  
White Dwarf ◽  
High Field ◽  
Space Telescope

scholarly journals [ITAL]Hubble Space Telescope[/ITAL] Observations of the Dwarf Nova WZ Sagittae: A Very Rapidly Rotating White Dwarf

1997 ◽  
Vol 484 (2) ◽  
pp. L149-L152 ◽  
Author(s):  
F. H. Cheng ◽  
Edward M. Sion ◽  
Paula Szkody ◽  
Min Huang
Keyword(s):  
White Dwarf ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Dwarf Nova

Hubble Space Telescope Observations of White Dwarf Stars

1993 ◽  
pp. 295-302
Author(s):  
Harry L. Shipman ◽  
Maurice Barnhill ◽  
Howard Bond ◽  
Fred Bruhweiler ◽  
David Finley ◽  
...  
Keyword(s):  
White Dwarf ◽  
Hubble Space Telescope ◽  
Dwarf Stars ◽  
Space Telescope ◽  
White Dwarf Stars

scholarly journals The HST large programme on NGC 6752 – III. Detection of the peak of the white dwarf luminosity function

2019 ◽  
Vol 488 (3) ◽  
pp. 3857-3865
Author(s):  
L R Bedin ◽  
M Salaris ◽  
J Anderson ◽  
M Libralato ◽  
D Apai ◽  
...  
Keyword(s):  
Globular Cluster ◽  
White Dwarf ◽  
Luminosity Function ◽  
Main Sequence ◽  
Hubble Space Telescope ◽  
Horizontal Branch ◽  
Space Telescope

ABSTRACT We report on the white dwarf (WD) cooling sequence of the old globular cluster NGC 6752, which is chemically complex and hosts a blue horizontal branch. This is one of the last globular cluster WD cooling sequences accessible to imaging by the Hubble Space Telescope. Our photometry and completeness tests show that we have reached the peak of the luminosity function of the WD cooling sequence, at a magnitude mF606W  = 29.4 ± 0.1, which is consistent with a formal age of ∼14 Gyr. This age is also consistent with the age from fits to the main-sequence turn-off (13–14 Gyr), reinforcing our conclusion that we observe the expected accumulation of WDs along the cooling sequence.

scholarly journals Preliminary analysis of a Hubble FOS spectrum of VW Hyi in quiescence: A DAZQ white dwarf and accretion belt/ring

1996 ◽  
Vol 158 ◽  
pp. 249-250
Author(s):  
E. M. Sion ◽  
M. Huang ◽  
F. H. Cheng ◽  
I. Hubeny ◽  
P. Szkody
Keyword(s):  
White Dwarf ◽  
Preliminary Analysis ◽  
Hubble Space Telescope ◽  
Uv Spectrum ◽  
Space Telescope ◽  
Dwarf Nova ◽  
Faint Object ◽  
Faint Object Spectrograph

AbstractWe present a preliminary analysis of the UV spectrum of the dwarf nova VW Hyi during early quiescence, obtained with the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST). The data were obtained approximately one day after the end of a normal outburst.

scholarly journals Hubble Space Telescope Far-UV Spectroscopy of the Short Orbital Period Recurrent Nova CI Aql: Implications for White Dwarf Mass Evolution

2019 ◽  
Vol 872 (1) ◽  
pp. 68
Author(s):  
Edward M. Sion ◽  
R. E. Wilson ◽  
Patrick Godon ◽  
Sumner Starrfield ◽  
Robert E. Williams ◽  
...  
Keyword(s):  
Orbital Period ◽  
White Dwarf ◽  
Hubble Space Telescope ◽  
Uv Spectroscopy ◽  
Space Telescope ◽  
Recurrent Nova

scholarly journals EUVE J0317 — 855: a rapidly rotating, high-field magnetic white dwarf

1997 ◽  
Vol 292 (2) ◽  
pp. 205-217 ◽  
Author(s):  
Lilia Ferrario ◽  
S. Vennes ◽  
D. T. Wickramasinghe ◽  
J. A. Bailey ◽  
D. J. Christian
Keyword(s):  
White Dwarf ◽  
High Field

A Hubble Space Telescope study of the underlying white dwarf in the dwarf nova VW Hydri during quiescence

1995 ◽  
Vol 444 ◽  
pp. L97 ◽  
Author(s):  
Edward M. Sion ◽  
Paula Szkody ◽  
Fu-Hua Cheng ◽  
Min Huang
Keyword(s):  
White Dwarf ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Dwarf Nova

scholarly journals The quest for planets around subdwarfs and white dwarfs from Kepler space telescope fields

2020 ◽  
Vol 642 ◽  
pp. A105
Author(s):  
J. Krzesinski ◽  
A. Blokesz ◽  
M. Siwak ◽  
G. Stachowski
Keyword(s):  
Time Series ◽  
White Dwarf ◽  
White Dwarfs ◽  
Series Data ◽  
Type B ◽  
Single Star ◽  
Space Telescope ◽  
Common Envelope ◽  
Short Period ◽  
Red Giant

Context. In this study, we independently test the presence of an exoplanet around the binary KIC 9472174, which is composed of a red dwarf and a pulsating type B subdwarf. We also present the results of our search for Jupiter-mass objects orbiting near to the eclipsing binary KIC 7975824, which is composed of a white dwarf and type B subdwarf, and the pulsating white dwarf KIC 8626021. Aims. The goal is to test analytical techniques and prepare the ground for a larger search for possible substellar survivors on tight orbits around post-common envelope binaries and stars at the end of their evolution, that is, extended horizontal branch stars and white dwarfs. We, therefore, mainly focus on substellar bodies orbiting these stars within the range of the host’s former red-giant or asymptotic-giant phase envelopes. Due to the methods we use, the quest is restricted to single-pulsating type B subdwarf and white dwarf stars and short-period eclipsing binaries containing a white dwarf or a subdwarf component. Methods. Our methods rely on the detection of exoplanetary signals hidden in photometric time series data from the Kepler space telescope, and they are based on natural clocks within the data itself, such as stellar pulsations and eclipse times. The light curves are analyzed using Fourier transforms, time-delays, and eclipse timing variations. Results. Based on the three objects studied in this paper, we demonstrate that these methods can be used to detect giant exoplanets orbiting around pulsating white dwarf or type B subdwarf stars as well as short-period binary systems, at distances which fall within the range of the former red-giant envelope of a single star or the common envelope of a binary. Using our analysis techniques, we reject the existence of a Jupiter-mass exoplanet around the binary KIC 9472174 at the distance and orbital period previously suggested in the literature. We also found that the eclipse timing variations observed in the binary might depend on the reduction and processing of the Kepler data. The other two objects analyzed in this work do not have Jupiter mass exoplanets orbiting within 0.7–1.4 AU from them, or larger-mass objects on closer orbits (the given mass limits are minimum masses). Conclusions. Depending on the detection threshold of the time-delay method and the inclination of the exoplanet orbit toward the observer, data from the primary Kepler mission allows for the detection of bodies with a minimum of ~1 Jupiter-mass orbiting these stars at ~1 AU, while data from the K2 mission extends the detection of objects with a minimum mass of ~7 Jupiter-mass on ~0.1 AU orbits. The exoplanet mass and orbital distance limits depend on the length of the available photometric time series.

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