Simulation of the visual light curve of CAL 87

2007 ◽  
pp. 53-64 ◽  
Author(s):  
S. Schandl ◽  
E. Meyer-Hofmeister ◽  
F. Meyer
Keyword(s):  
Light Curve ◽  
Visual Light

Visual Light-Curve of Nova Puppis.

1943 ◽  
Vol 97 ◽  
pp. 443
Author(s):  
Gerard P. Kuiper
Keyword(s):  
Light Curve ◽  
Visual Light

scholarly journals IRAS LRS Spectral Class and Light Curve of M & S Miras

1989 ◽  
Vol 106 ◽  
pp. 292-292
Author(s):  
M.S. Vardya
Keyword(s):  
Light Curve ◽  
Mean Amplitude ◽  
Asymmetry Factor ◽  
Necessary Condition ◽  
Infrared Excess ◽  
Strong Emission ◽  
Spectral Class ◽  
Increase With Increase ◽  
The Mean ◽  
Visual Light

A large sample of 177 Miras, comprising 164 M and 13 S stars, has been examined to determine the dependence of 9.7 μm silicate emission, as revealed by their IRAS LRS Spectral class, on the visual light curve asymmetry factor, f. It is found that the silicate feature occurs not only in M (Vardya et al. 1986; Onaká & de Jong 1987) but in S Miras also only for f ≤ 0.45. This, however, is only a necessary condition, as about one fifth of Miras with f ≤ 0.45 do not show the 9.7 μm emission. This non-detection shows dependence on other parameters like the mean visual light amplitude. Non-detection is highest in the region 0.43 < f ≤ 0.45, as well as when mean amplitude is ≤ 5m.0. Though strong emission features in M Miras may occur for any value of f, very weak features are absent for small values of f, and the strongest feature tends to appear for large values of f. Infrared excess tends to increase with increase in the strength of the silicate emission and with decrease in the value of f.

Some Dependences for Long-Period Variables and a Possible Scheme of their Evolution

1989 ◽  
Vol 131 ◽  
pp. 451-451
Author(s):  
I. L. Andronov ◽  
L. S. Kudashkina ◽  
G. M. Rudnitskij
Keyword(s):  
Light Curve ◽  
Color Index ◽  
Variable Stars ◽  
Maser Emission ◽  
Long Period ◽  
General Catalogue ◽  
Long Period Variables ◽  
Molecular Lines ◽  
Visual Light

Some dependences between the parameters for approximately 150 stars, of which 81 are sources of maser emission in molecular lines, are constructed. The following parameters are considered: period P, asymmetry (M-m) of the visual light curve, visual amplitude A, color index (I-K). We use the data of the General Catalogue of Variable Stars. For the stars Z Cyg, R Tau, R Peg, RT Vir, RX Boo, PZ Cas, U Her, and R Cas, some parameters were determined by the authors.

scholarly journals Infrared Observations of Nova Aquilae 1982

1983 ◽  
Vol 72 ◽  
pp. 121-125
Author(s):  
M.F. Bode ◽  
J.K. Davies ◽  
A. Evans ◽  
D.C.B. Whittet
Keyword(s):  
Light Curve ◽  
Decay Rate ◽  
South African ◽  
Astronomical Observatory ◽  
Infrared Photometry ◽  
Dust Shell ◽  
The South ◽  
Infrared Observations ◽  
Spectroscopic Observations ◽  
Visual Light

AbstractWe describe infrared photometry and spectroscopy of Nova Aquilae 1982. The broadband observations suggest that the dust shell of Nova Aquilae was anomalous, while the spectroscopic observations point to the presence of molecules in the nova environment.Nova Aquilae was discovered (Honda 1982) on 1982 January 27th. The visual light curve, based on visual estimates (IAU circulars), IUE FES counts (derived assuming (B-V) = 0) and photometry at the South African Astronomical Observatory (SAA0), suggest a fast nova with visual decay rate mv = 0.3 mag d-1. Spectral development and outburst amplitude suggest that the nova was discovered at maximum.

scholarly journals Dust Obscuration Events of the Symbiotic Nova RR Tel in the Near IR

2004 ◽  
Vol 194 ◽  
pp. 225-225
Author(s):  
D. Kotnik-Karuza ◽  
M. Friedjung ◽  
P. A. Whitelock
Keyword(s):  
Light Curve ◽  
White Dwarf ◽  
Light Curves ◽  
Near Ir ◽  
Ir Photometry ◽  
Visual Light

By use of ground based IR photometry, we have studied the dust obscuration events of the symbiotic nova RR Tel which is a binary composed of a cool mira and a hot white dwarf. The JHKL light curves were corrected for Mira pulsations and correlated to the AAVSO visual light curve. We compare the behaviour of the three obscurations in different wavelength bands and propose interpretations of the results.

scholarly journals Spectral Evolution of Nova Vulpeculae 1976

1977 ◽  
Vol 42 ◽  
pp. 182-184
Author(s):  
P. Rafanelli ◽  
A. Vittone
Keyword(s):  
Light Curve ◽  
Color Index ◽  
Mean Value ◽  
Spectral Evolution ◽  
Slow Recovery ◽  
Gradual Decline ◽  
Visual Magnitude ◽  
The Mean ◽  
Visual Light

Nova Vulpeculae 1976 was discovered by G.E.D. Alcock (1976) on October 21, 1976 as a star of visual magnitude 6.5 in position (1950): The visual light curve, plotted together with the color index B-V in fig.1, was obtained using the observations published in the I.A.U. Circulars. It shows a slow fall from maximum, about 2.5 magnitudes in 60 days, with characteristic fluctuations, an abrupt drop of about 3.5 magnitudes in 24 days, a slow recovery of one magnitude in 30 days, and a very gradual decline to minimum. The color index B-V remained almost constant near the mean value +1.1 during the slow early decline.

scholarly journals Insights into the inner regions of the FU Orionis disc

2018 ◽  
Vol 618 ◽  
pp. A79 ◽  
Author(s):  
Michał Siwak ◽  
Maciej Winiarski ◽  
Waldemar Ogłoza ◽  
Marek Dróżdż ◽  
Stanisław Zoła ◽  
...  
Keyword(s):  
Light Curve ◽  
Spectral Range ◽  
Small Amplitude ◽  
Winter Season ◽  
Stellar Mass ◽  
Periodic Oscillations ◽  
Clear Sign ◽  
Fu Ori ◽  
Periodic Family ◽  
Visual Light

Context. We investigate small-amplitude light variations in FU Ori occurring in timescales of days and weeks. Aims. We seek to determine the mechanisms that lead to these light changes. Methods. The visual light curve of FU Ori gathered by the MOST satellite continuously for 55 d in the 2013–2014 winter season and simultaneously obtained ground-based multi-colour data were compared with the results from a disc and star light synthesis model. Results. Hotspots on the star are not responsible for the majority of observed light variations. Instead, we found that the long periodic family of 10.5–11.4 d (presumably) quasi-periods showing light variations up to 0.07 mag may arise owing to the rotational revolution of disc inhomogeneities located between 16 and 20 R⊙. The same distance is obtained by assuming that these light variations arise because of a purely Keplerian revolution of these inhomogeneities for a stellar mass of 0.7 M⊙. The short-periodic (∼3 – 1.38 d) small amplitude (∼0.01 mag) light variations show a clear sign of period shortening, similar to what was discovered in the first MOST observations of FU Ori. Our data indicate that these short-periodic oscillations may arise because of changing visibility of plasma tongues (not included in our model), revolving in the magnetospheric gap and/or likely related hotspots as well. Conclusions. Results obtained for the long-periodic 10–11 d family of light variations appear to be roughly in line with the colour-period relation, which assumes that longer periods are produced by more external and cooler parts of the disc. Coordinated observations in a broad spectral range are still necessary to fully understand the nature of the short-periodic 1–3 d family of light variations and their period changes.

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