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Fressin, F.; Guillot, T.; Schmider, F.-X.; Agabi, A.; Moutou, C.; Aigrain, S.; Bouchy, F.; Boer, M.; Pont, F.; Erikson, A.; Rauer, H.; The A Step Team. (2007). A STEP: Towards a Large Photometric Survey for Exoplanets at Dome C (Vol. 25).
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Vernin, J.; Chadid, M.; Aristidi, E.; Agabi, A.;Trinquet, H.; van der Swaelmen, M. (2009). First single star scidar measurements at Dome C, Antarctica. ASTRONOMY & ASTROPHYSICS, 500(3), 1271–1276.
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Zinnecker H., Epchtein N., Rauer H., (eds.). (2008). (Vol. 33).
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Spinoglio L. , Epchtein N. (eds.). (2010). 3rd ARENA Conference: An Astronomical Observatory at CONCORDIA (Dome C, Antarctica) Frascati, Italy, May 11-15, 2009.
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Epchtein N., Candidi, M. (2007). Proc. 1st ARENA Conference on “Large Astronomical Infrastructures at CONCORDIA, prospects and constraints for Antarctic Optical/IR Astronomy”, EAS Publications Series (Vol. 25).
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Fossat Eric, Aristidi Eric, Agabi Karim, Bondoux Erick, Challita Zalpha, Jeanneaux Francois, Mekarnia Djamel, . (2010). Typical duration of good seeing sequences at Concordia
. ASTRONOMY & ASTROPHYSICS, 517A, 4.
Abstract: Context: The winter seeing at Concordia is essentially bimodal, excellent or quite poor, with relative proportions that depend on altitude above the snow surface. This paper studies the temporal behavior of the good seeing sequences. Aims: An efficient exploitation of extremely good seeing with an adaptive optics system needs long integrations. It is then important to explore the temporal distribution of the fraction of time providing excellent seeing. Methods: Temporal windows of good seeing are created by a simple binary process. Good or bad. Their autocorrelations are corrected for those of the existing data sets, since these are not continuous, being often interrupted by technical problems in addition to the adverse weather gaps. At the end these corrected autocorrelations provide the typical duration of good seeing sequences. This study has to be a little detailed as its results depend on the season, summer or winter. Results: Using a threshold of 0.5 arcsec to define the “good seeing”, three characteristic numbers are found to describe the temporal evolution of the good seeing windows. The first number is the mean duration of an uninterrupted good seeing sequence: it is $\tau0=7.5$ hours at 8 m above the ground (15 hours at 20 m). These sequences are randomly distributed in time, with a negative exponential law of damping time $\tau1=29$ hours (at elevation 8 m and 20 m). The third number is the mean time between two 29 hours episodes. It is T=10 days at 8 m high (5 days at 20 m).
Keywords: Instrumentation and Methods for Astrophysics,
Programme: 908
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Chadid M, Vernin J, Mekarnia D, Chapellier E, Trinquet H, Bono G, . (2010). First Antarctica light curve. PAIX monitoring of the Blazhko RR Lyrae star: S Arae. A&A, 516, 15.
Abstract: Context. In the context of long and continuous time-series photometry and after the MOST, CoRoT, KEPLER space missions and large geographic longitude ground-based networks, a new method is offered by the polar location helping to cope with the problem associated with the Earth's day-night cycle.
Aims: We present the first long time -series photometry from Dome Charlie in the heart of Antarctica and analyze ~4400 photometric measurements of RR Lyrae star S Arae obtained in July and August 2007.
Methods: The 40-cm telescope and Photometer AntarctIca eXtinction named PAIX were used for long photometric measurements with high time resolution and a duty cycle of 65%. The Fourier technique was used for the frequency analysis. New high-precision spectroscopic observations of S Arae were also collected using HARPS over one pulsation cycle of S Arae.
Results: We confirm the known radial fundamental period of 0.452 day. The high order of its harmonics shows the nonlinear nature of the radial mode. The Blazhko modulation is directly detected in the spectrum and shows a value around 48 d. Together with the Blazhko frequency we also detected triplet structure components up to 15th order showing a nonlinear behavior of the Blazhko modulation. Thus, we conclude that S Arae is a bona fide Blazhko star. The data reveal that there are irregular changes in the S Arae atmosphere during the Blazhko cycle. A residual scatter phenomenon is detected and is more intense where the nonlinear effects are strongest. Therefore, the connection between temporal hydrodynamic phenomena and such modulation has to be taken into account in Blazhko models.
Conclusions: High-precision CCD photometry with a very good time resolution can be undertaken at Dome Charlie in Antarctica, and it helps to complete astrophysical measurement time-series.
Programme: 908
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Brauer P., Risbo T., Merayo J.M.G. & Nielsen O.V. (2000). Fluxgate Sensor for the Vector Magnetometer Onboard The 'Astrid-2' Satellite. Sensors and actuators a-physical, 81, 184–188.
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Glassmeier K.H., Musmann G., Weeks C. & Envielle M. (2000). Mars – A planet in magnetic transition? Planetary and space science, 48, 1153–1160.
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