M. Candidi

Institute for Space Astrophysics and Planetology

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S. Orsini

Institute for Space Astrophysics and Planetology

H. Balsiger

University of Bern

M. F. Marcucci

National Institute for Astrophysics

Igor Bertello

Institute for Space Astrophysics and Planetology

M. Stokholm

University of Bern

E. Amata

Institute for Space Astrophysics and Planetology

Piero Diego

National Institute for Astrophysics

S. Massetti

National Institute for Astrophysics

P. Ubertini

Institute for Space Astrophysics and Planetology

P. Ballatore

Istituto di Scienza e Tecnologie dell'Informazione "Alessandro Faedo"

Cooperative Institutions

National Institute for Astrophysics

Centre National de la Recherche Scientifique

Institute for Space Astrophysics and Planetology

Istituto Nazionale di Fisica Nucleare

University of Rome Tor Vergata

UNSW Sydney

Johns Hopkins University Applied Physics Laboratory

California Institute of Technology

Chinese Academy of Sciences

Sapienza University of Rome

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The Gattini Cameras for Optical Sky Brightness Measurements at Dome C, Antarctica

EAS Publications Series (2007)

Anna Moore É. Aristidi M. C. B. Ashley Runa Briguglio M. Busso

The Gattini cameras are two site testing instruments for the measurement of optical sky brightness, large area cloud cover and auroral detection of the night sky above the high altitude Dome C site in Antarctica. The cameras have been operating since installation in January 2006 and are currently at the end of the first Antarctic winter season. The cameras are transit in nature and are virtually identical, both adopting Apogee Alta CCD detectors. By taking frequent images of the night sky we obtain long term cloud cover statistics, measure the sky background intensity as a function of solar and lunar altitude and phase and directly measure the spatial extent of bright aurora if present and when they occur. The full data set will return in December 2006 however a limited amount of data has been transferred via the Iridium network enabling preliminary data reduction and system evaluation. An update of the project is presented together with preliminary results from data taken since commencement of the winter season.

Sky brightness

Night sky

10.1051/eas:2007069

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Citations (2)

The RETE and TEMAG experiments for the TSS missions

M. Candidi M. Dobrowolny F. Mariani

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Discrimination between Internal and External origin contributions from LEO satellite magnetic field data.

cosp (2018)

Mirko Piersanti P. Ubertini Piero Diego Igor Bertello Massimo Materassi

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Auroral observations at the Mario Zucchelli Base (Antarctica). Morphological features.

MmSAI (2009)

Giuseppe Consolini E. P. Balsamo M. Candidi Paola De Michelis M. F. Marcucci

Auroral displays are the visible manifestation of the solar wind-magnetosphereionosphere interaction at the high latitude polar regions. The study of this phenomenon is very relevant for both the investigation of the magnetosphere-ionosphere coupling and the comprehension of the overall magnetospheric dynamics during the so-called magnetic substorms. Here, we present some preliminary results on the morphological features of the auroral emission as observed at the Mario Zucchelli station in Antarctica during a recent winter campaign. In particular, we are going to show how the morphology of the auroral emission changes with the wavelength (630.0 nm, 557.7 nm and 427.8 nm).

High latitude

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On a Possible Relationship Between Atmospheric Dynamics Ozone and Global Auroral Activity

International Cosmic Ray Conference (1995)

M. F. Marcucci S. Orsini M. Candidi M. Storini

Atmospheric Dynamics

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Intensity distribution of dayside polar soft electron precipitation and the IMF

Planetary and Space Science (1983)

M. Candidi H. W. Kroehl C.‐I. Meng

Substorm

Noon

Electron precipitation

Intensity

Local time

10.1016/0032-0633(83)90040-5

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Citations (33)

Cold streams of ionospheric oxygen in the plasma sheet during the CDAW 6 event of March 22, 1979

Journal of Geophysical Research Atmospheres (1985)

S. Orsini E. Amata M. Candidi H. Balsiger M. Stokholm

During the March 22, 1979, substorm events the positive ion experiment on ISEE 2 (EGD) detected intense streams of low‐energy ions (mostly between 50 and 500 eV) moving tailward in the near‐earth magnetotail. The first clear observation of these streams was made about 30 min after the onset of the first substorm. On the basis of a comparison with simultaneous data from the ion composition experiment on ISEE 1, which was trailing ISEE 2 in the same orbit by about 2 R E , it is argued that these streams consisted primarily of O + ions. From the analysis of the direction and energy of the streams we draw the following conclusions: (1) In addition to the bulk velocity along the magnetic field lines the streams also have a significant and varying perpendicular velocity due to E × B/B ² drift. The GSE x and y components of the E × B/B ² drift are generally toward the center of the magnetotail in the lobe and toward the tail flanks in the plasma sheet, in qualitative agreement with the field topology one obtains by mapping the north‐south electric field from the morning and evening auroral ovals well into the distant magnetotail, in a manner previously proposed in the literature. (2) The O + flow speed and flow direction, as well as density and temperature, undergo strong fluctuations during the course of the two substorms. Some of these fluctuations seem to reflect an increased outflux of ionospheric O + in connection with increasing magnetic activity, while others may be related to magnetotail movements. Certain oscillations of the flow direction and speed with periods ranging from 10 to 15 min may suggest a wavelike boundary between the plasma sheet and the lobes.

Substorm

Plasma sheet

10.1029/ja090ia05p04091

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Citations (20)

"ROMOLO E REMO": Scientific Proposal for a Two-Satellite Magnetospheric Mission

M. Candidi S. Orsini

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Use of hydromagnetic waves to map geomagnetic field lines

Journal of Geophysical Research Atmospheres (1981)

R. A. Greenwald A. D. M. Walker M. Candidi

Quasi‐periodic oscillations in magnetospheric electric and magnetic fields are communicated to the ionosphere via guided Alfvén waves, propagating along magnetic field lines. Thus, if one could identify ionospheric and magnetospheric regions showing highly correlated temporal variations, one would, in effect, have determined the region in the ionosphere conjugate to a given location in the magnetosphere. In this paper we present a cross correlation analysis of Pc 5 magnetic field oscillations observed by GEOS 2 with drift velocity oscillations (electric field) observed with the STARE radars in the ionosphere. GEOS 2 is in geostationary orbit with its conjugate point nominally located in the STARE field of view. Several comparisons were made over a one hour period in the early afternoon sector and correlation coefficients reaching 0.84 over a limited area in the ionosphere were obtained. Between the beginning and end of the hour, the measured footpoint was displaced by ∼ 1° in latitude and ∼2.5° in longitude. Neither of the two determinations agreed with the predictions of the Mead‐Fairfield or Olson‐Pfitzer models, although the difference at the end of the hour was of the same order as the dispersion between the two models.

Field line

Longitude

Ionospheric dynamo region

Conjugate points

Local time

10.1029/ja086ia13p11251

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Citations (27)

Ionospheric streams at altitudes below 14RE

Unknow (1985)

S. Orsini M. Candidi

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