دورية أكاديمية
Sky Brightness Evaluation and First Coronal Signal Detection from Concordia Base (Antarctica) with a Calibrated Micropolarizer Array Camera.
| العنوان: | Sky Brightness Evaluation and First Coronal Signal Detection from Concordia Base (Antarctica) with a Calibrated Micropolarizer Array Camera. |
|---|---|
| المؤلفون: | Liberatore, Alessandro, Capobianco, Gerardo, Fineschi, Silvano, Massone, Giuseppe, Zangrilli, Luca, Susino, Roberto, Nicolini, Gianalfredo |
| المصدر: | Solar Physics; Oct2023, Vol. 298 Issue 10, p1-17, 17p |
| مصطلحات موضوعية: | SKY brightness, SOLAR magnetic fields, SIGNAL detection, SOLAR atmosphere, SEA level, SOLAR corona, DAYLIGHT |
| مصطلحات جغرافية: | HAWAII, ANTARCTICA |
| مستخلص: | The solar corona is the outer layer of the Sun's atmosphere. The brightness of the solar corona is a million times lower than that of the solar disk. The Earth's sky brightness itself is high enough to cover the coronal signal during ground-based observations. For this reason, the study of sky characteristics plays a fundamental role in observing the solar corona. To date, the only place with the sky characteristics that allow continuous coronagraphic measurements from Earth is at the MLO (Mauna Loa Observatory; Hawaii, ≈ 3400 m above sea level). This paper shows the results obtained as part of the "Extreme Solar Coronagraphy Antarctic Program Experiment" (ESCAPE) at Concordia Base, Antarctica (Dome C plateau-coord.: 75∘06′ S, 123∘20′ E, ≈ 3300 m above sea level) during the 37th campaign and gives a summary of all the sky-brightness measurements obtained from this site (34th and 35th campaigns). Dome C is confirmed to be a coronagraphic site with a sky brightness of about 1 × 10 − 6 B ⊙ . For the first time, it was also possible to detect a coronal signal and to compare it with what was measured by the COronal Solar Magnetism Observatory (COSMO) K-coronagraph (K-Cor) at the MLO. All these results were obtained by using a micropolarizer camera mounted within a coronagraph designed for Antarctic environments. [ABSTRACT FROM AUTHOR] |
| Copyright of Solar Physics is the property of Springer Nature and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.) | |
| قاعدة البيانات: | Complementary Index |
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