Infrared Light Curves and Absolute Parameters of the Active Binary RT Andromedae

1995 ◽  
Vol 110 ◽  
pp. 1376 ◽  
Author(s):  
M. J. Arevalo ◽  
C. Lazaro ◽  
A. Claret
Keyword(s):  
Light Curves ◽  
Infrared Light ◽  
Absolute Parameters

scholarly journals Interpreting the Evolving Clumpy Shell Structure of IRC +10216 in Terms of Time Dependent Dust Shell Models

2003 ◽  
Vol 209 ◽  
pp. 127-128
Author(s):  
J. M. Winters ◽  
T. Blöcker ◽  
K.-H. Hofmann ◽  
G. Weigelt
Keyword(s):  
Time Scale ◽  
High Spatial Resolution ◽  
Light Curves ◽  
Infrared Light ◽  
Pulsation Period ◽  
Line Profiles ◽  
Dust Shell ◽  
Time Intervals ◽  
Stellar Pulsation ◽  
Shell Models

The prototypical dust-enshrouded carbon Mira IRC +10216 is known to exhibit intrinsic changes on a time scale of the order of only a few years as revealed, e.g., by CO infrared line profiles (Winters et al. 2000a), its infrared light curves, and by high spatial resolution monitoring in the infrared (Osterbart et al. 2000; Tuthill et al. 2000). In particular, the infrared light curves indicate a possible periodicity on a ≈ 20 yr time scale, i.e. that a recurrent phenomenon might lead to the observed variations. Such multi-periodicity time scales of several (≈ 10) stellar pulsation periods are predicted by consistent hydrodynamical models which include a proper treatment of dust formation (e.g. Winters et al. 2000b). In these models discrete dust layers form in time intervals which are several times longer than the typical pulsation period of an AGB star (Fleischer, Gauger, & Sedlmayr 1995; Höfner, Feuchtinger, & Dorfi 1995).

scholarly journals NEAR-INFRARED LIGHT CURVES OF THE BROWN DWARF ECLIPSING BINARY 2MASS J05352184-0546085: CAN SPOTS EXPLAIN THE TEMPERATURE REVERSAL?

2009 ◽  
Vol 699 (2) ◽  
pp. 1196-1208 ◽  
Author(s):  
Yilen Gómez Maqueo Chew ◽  
Keivan G. Stassun ◽  
Andrej Prša ◽  
Robert D. Mathieu
Keyword(s):  
Near Infrared ◽  
Light Curves ◽  
Infrared Light ◽  
Brown Dwarf ◽  
Near Infrared Light ◽  
Eclipsing Binary

Infrared Light Curves and Spectroscopic Classification of the Algol System UX HER

1997 ◽  
Vol 113 ◽  
pp. 1122 ◽  
Author(s):  
C. Lazaro ◽  
I. G. Martinez-Pais ◽  
M. J. Arevalo ◽  
E. Antonopoulou
Keyword(s):  
Light Curves ◽  
Infrared Light ◽  
Algol System

scholarly journals Infrared light curves of the dwarf nova Z Chamaeleontis

1981 ◽  
Vol 196 (2) ◽  
pp. 121-128 ◽  
Author(s):  
J. Bailey ◽  
M. R. Sherrington ◽  
A. B. Giles ◽  
R. F. Jameson
Keyword(s):  
Light Curves ◽  
Infrared Light ◽  
Dwarf Nova

scholarly journals The Optical/Near‐Infrared Light Curves of SN 2002ap for the First 140 Days after Discovery

2003 ◽  
Vol 592 (1) ◽  
pp. 467-474 ◽  
Author(s):  
Yuzuru Yoshii ◽  
Hiroyuki Tomita ◽  
Yukiyasu Kobayashi ◽  
Jinsong Deng ◽  
Keiichi Maeda ◽  
...  
Keyword(s):  
Near Infrared ◽  
Light Curves ◽  
Infrared Light ◽  
Near Infrared Light

scholarly journals Asteroid models reconstructed from the Lowell Photometric Database and WISE data

2018 ◽  
Vol 617 ◽  
pp. A57 ◽  
Author(s):  
J. Ďurech ◽  
J. Hanuš ◽  
V. Alí-Lagoa
Keyword(s):  
Joint Inversion ◽  
Rotation Period ◽  
Thermal Infrared ◽  
Light Curves ◽  
Physical Models ◽  
Infrared Light ◽  
Inversion Method ◽  
Significant Discrepancy ◽  
Wide Range ◽  
New Models

Context. Information about the spin state of asteroids is important for our understanding of the dynamical processes affecting them. However, spin properties of asteroids are known for only a small fraction of the whole population. Aims. To enlarge the sample of asteroids with a known rotation state and basic shape properties, we combined sparse-in-time photometry from the Lowell Observatory Database with flux measurements from NASA’s WISE satellite. Methods. We applied the light curve inversion method to the combined data. The thermal infrared data from WISE were treated as reflected light because the shapes of thermal and visual light curves are similar enough for our purposes. While sparse data cover a wide range of geometries over many years, WISE data typically cover an interval of tens of hours, which is comparable to the typical rotation period of asteroids. The search for best-fitting models was done in the framework of the Asteroids@home distributed computing project. Results. By processing the data for almost 75 000 asteroids, we derived unique shape models for about 900 of them. Some of them were already available in the DAMIT database and served us as a consistency check of our approach. In total, we derived new models for 662 asteroids, which significantly increased the total number of asteroids for which their rotation state and shape are known. For another 789 asteroids, we were able to determine their sidereal rotation period and estimate the ecliptic latitude of the spin axis direction. We studied the distribution of spins in the asteroid population. Apart from updating the statistics for the dependence of the distribution on asteroid size, we revealed a significant discrepancy between the number of prograde and retrograde rotators for asteroids smaller than about 10 km. Conclusions. Combining optical photometry with thermal infrared light curves is an efficient approach to obtaining new physical models of asteroids. The amount of asteroid photometry is continuously growing and joint inversion of data from different surveys could lead to thousands of new models in the near future.

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