1,211 research outputs found
Understanding CME and associated shock in the solar corona by merging multi wavelengths observation
Using multi-wavelength imaging observations, in EUV, white light and radio,
and radio spectral data over a large frequency range, we analyzed the
triggering and development of a complex eruptive event. This one includes two
components, an eruptive jet and a CME which interact during more than 30 min,
and can be considered as physically linked. This was an unusual event. The jet
is generated above a typical complex magnetic configuration which has been
investigated in many former studies related to the build-up of eruptive jets;
this configuration includes fan-field lines originating from a corona null
point above a parasitic polarity, which is embedded in one polarity region of
large Active Region (AR). The initiation and development of the CME, observed
first in EUV, does not show usual signatures. In this case, the eruptive jet is
the main actor of this event. The CME appears first as a simple loop system
which becomes destabilized by magnetic reconnection between the outer part of
the jet and the ambient medium. The progression of the CME is closely
associated with the occurrence of two successive types II bursts from distinct
origin. An important part of this study is the first radio type II burst for
which the joint spectral and imaging observations allowed: i) to follow, step
by step, the evolution of the spectrum and of the trajectory of the radio
burst, in relationship with the CME evolution; ii) to obtain, without
introducing an electronic density model, the B-field and the Alfven speed.Comment: 17 pages, 13 figure
Classifications of elliptic fibrations of a singular K3 surface
We classify, up to automorphisms, the elliptic fibrations on the singular K3
surface whose transcendental lattice is isometric to .Comment: 28 page
In-flight calibration of STEREO-B/WAVES antenna system
The STEREO/WAVES (SWAVES) experiment on board the two STEREO spacecraft
(Solar Terrestrial Relations Observatory) launched on 25 October 2006 is
dedicated to the measurement of the radio spectrum at frequencies between a few
kilohertz and 16 MHz. The SWAVES antenna system consists of 6 m long orthogonal
monopoles designed to measure the electric component of the radio waves. With
this configuration direction finding of radio sources and polarimetry (analysis
of the polarization state) of incident radio waves is possible. For the
evaluation of the SWAVES data the receiving properties of the antennas,
distorted by the radiation coupling with the spacecraft body and other onboard
devices, have to be known accurately. In the present context, these properties
are described by the antenna effective length vectors. We present the results
of an in-flight calibration of the SWAVES antennas using the observations of
the nonthermal terrestrial auroral kilometric radiation (AKR) during STEREO
roll maneuvers in an early stage of the mission. A least squares method
combined with a genetic algorithm was applied to find the effective length
vectors of the STEREO Behind (STEREO-B)/WAVES antennas in a quasi-static
frequency range () which fit best to the model
and observed AKR intensity profiles. The obtained results confirm the former
SWAVES antenna analysis by rheometry and numerical simulations. A final set of
antenna parameters is recommended as a basis for evaluations of the SWAVES
data
Reply to comment by B. Cecconi on "Spectral features of SKR observed by Cassini/RPWS: Frequency bandwidth, flux density and polarization"
International audienceThe main purpose of the paper by Galopeau et al.[2007] was to classify the spectral features of the Saturniankilometric radiation (SKR) starting from three physicalobserved parameters: the frequency bandwidth, the fluxdensity, and the pol arization. We show in the presentresponse that an unsupervised application of arbitrary auto-matic criteria during the data processing (such as a signal-to-noise ratio greater than 23 dB) can totally judge a weaknatural emission as a background noise. As a consequence,such a situation may lead to consideration of only the datapresenting a degree of circular polarization close to 100%and neglect a huge part of the data. Galopeau et al. [2007]considered a phenomenological aspect and gave an estima-tion of the Stokes parameters. This approach leads to firstrecognizing spectral components (flux density and band-width) in the frequency range from 3.5 kHz to 1200 kHz,and then deriving the Stokes parameters for each compo-nent. The Cassini/RPWS instrument provides long-lastingcoverage of radio emissions at Saturn with unprecedentedinstrumental capabilities
Radio pulses from cosmic ray air showers - Boosted Coulomb and Cherenkov fields
High-energy cosmic rays passing through the Earth's atmosphere produce
extensive showers whose charges emit radio frequency pulses. Despite the low
density of the Earth's atmosphere, this emission should be affected by the air
refractive index because the bulk of the shower particles move roughly at the
speed of radio waves, so that the retarded altitude of emission, the
relativistic boost and the emission pattern are modified. We consider in this
paper the contribution of the boosted Coulomb and the Cherenkov fields and
calculate analytically the spectrum using a very simplified model in order to
highlight the main properties. We find that typically the lower half of the
shower charge energy distribution produces a boosted Coulomb field, of
amplitude comparable to the levels measured and to those calculated previously
for synchrotron emission. Higher energy particles produce instead a
Cherenkov-like field, whose amplitude may be smaller because both the negative
charge excess and the separation between charges of opposite signs are small at
these energies.Comment: 10 figures - Accepted by Astronomy & Astrophysic
Radio Jupiter after Voyager: An overview of the Planetary Radio Astronomy observations
Jupiter's low frequency radio emission morphology as observed by the Planetary Radio Astronomy (PRA) instrument onboard the Voyager spacecraft is reviewed. The PRA measurement capabilities and limitations are summarized following over two years of experience with the instrument. As a direct consequence of the PRA spacecraft observations, unprecedented in terms of their sensitivity and frequency coverage, at least three previous unrecognized emission components were discovered: broadband and narrow band kilometric emission and the lesser arc decametric emission. Their properties are reviewed. In addition, the fundamental structure of the decameter and hectometer wavelength emission, which is believed to be almost exclusively in the form of complex but repeating arc structures in the frequency time domain, is described. Dramatic changes in the emission morphology of some components as a function of Sun-Jupiter-spacecraft angle (local time) are described. Finally, the PRA in suit measurements of the Io plasma torus hot to cold electron density and temperature ratios are summarized
Search for companions around Sirius
Since the discovery of Sirius-B about 130 yr ago, there have been several
claims of a possible second companion around the brightest star Sirius-A. Such
a companion could, in particular, be responsible of the suspected colour change
of the star, now strongly suggested from two independent historical sources. We
reported here on a new observation of the sky region around Sirius, to search
for such a companion, using a coronographic device.
By comparison of the new stellar field with a similar image obtained by us
13 yr ago and using the Sirius proper motion, we are able to eliminate
the most obvious companion candidates down to a magnitude m17 in a
field from 30 arcsec to 2.5 arcmin of the central star. None of the visible
stars appears consistent in magnitude and colours with what expected from
current theoretical models and observations of low-mass stars.
From the study of the same field, it is also shown that the Sirius companion,
consistently reported by observers during the years 1920-1930, is most probably
an unrelated m12 background star, now 1 arcmin away but
located precisely on the Sirius proper motion trajectory. The closest apparent
conjunction with Sirius was realized in 1937 with a minimum angular distance of
6.9 arcsec, of the same order than the Sirius A-B binary separation.
The reported observations do not eliminate the possibility of a second
companion but now confined the search to the more central 30 arcsec region
around Sirius. In particular, the existence of a long period companion cannot
definitively be ruled out since the arbitrary orientation of the orbit can
yield an observed projected position on sky inside this more central region.Comment: 6 pages, 4 figures, published in Astronomy and Astrophysic
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