Secchirh

Solar Orbiter

Renaud Romagnan — 2022-05-30T08:37:42Z

The Radio/Solar Orbiter (SolO) pages combine radio observations from ground and space with quick-look plots of X-ray light curves at selected photon energies from Solar Orbiter / STIX and time histories of the intensities of energetic electrons and protons in selected energy ranges from Solar Orbiter / EPD.

The plot on the top right indicates the relative position of Solar Orbiter with respect to the Sun-Earth axis on the given day. Please be aware that during certain periods, the view of the Sun provided by ground-based instruments cannot be directly compared to the observations from Solar Orbiter.

The Spectrometer/Telescope for Imaging X-rays (STIX) is described at https://datacenter.stix.i4ds.net/. The quick-look plots on the present web site are produced from low-latency data (not science data). They show the count time histories in 20s time intervals in three photon energy channels (4-10, 10-15, 15-25 keV). The time axis is the arrival time of photons at 1 AU, corrected from the light propagation time between the satellite and the earth using the coordinates of the spacecraft provided by the SPICE kernels.
The Energetic Particle Detector EPD is described at https://espada.uah.es/epd/ . The quick-look plots on the present web site show the time histories of protons (energy ranges 7.075-28.33 MeV, 47.05-104.8 MeV) and electrons (energy ranges 53-73 and 282-397 keV), drawn from low-latency data. The intensities are averages over the four viewing directions of EPD. The time axis is the time at the spacecraft.
The Radio and Plasma Waves instrument (RPW) is described at https://rpw-datacenter.obspm.fr/. The quick-look plots on this website are produced from calibrated science data products (L2), which include dynamical spectra acquired by the RPW TNR-HFR radio receivers between 4 kHz and 16.4 MHz. They show the power spectral density (in log scale) measured at the receiver level, as functions of UTC time and frequency (in MHz).

The data shown are quicklook-data, used for giving an overview of observations and a first guide to the event selection for scientific investigations. They are not suited for scientific publications. Please refer to the instrument web sites for advise on the recovery and use of science-ready data.

Learmonth spectrograph

Renaud Romagnan — 2018-07-12T09:30:07Z

For a description, see external link

Culgoora spectrograph

Renaud Romagnan — 2018-07-12T09:28:38Z

For a description, see external link

Gauribidanur Low-frequency Solar Spectrograph (GLOSS)

Renaud Romagnan — 2018-07-12T09:27:07Z

Contact persons :
R. Ramesh

Gauribidanur Low-frequency Solar Spectrograph (GLOSS) is operated by the Indian Institute of Astrophysics at the Gauribidanur radio observatory, about 100 km north of Bangalore. GLOSS is a dedicated instrument for obtaining dynamic spectrum of the transient emission from the solar corona. The antenna system consists of 8 log periodic dipoles (LPD).

Antenna : LPD
Frequency range : 40 - 440 MHz
Number of frequency points : 401
Spectral resolution : 1 MHz
Sweep time (40 - 440 MHz) : 250 ms
Observation duration : 02:30 to 11:30 UT (9 hr)
Location : 77° E 14° N

Link : https://www.iiap.res.in/centers/radio
Reference : Gauribidanur Low-frequency Solar Spectrograph P. Kishore, C. Kathiravan, R. Ramesh, M. Rajalingam, Indrajit V. Barve, 2014, Solar Physics, Vol. 289, pp. 3995-4005 https://link.springer.com/article/10.1007/s11207-014-0539-1

Humain spectrograph

Renaud Romagnan — 2018-07-12T09:26:31Z

Contact person : C. Marque

Observations from Humain (Belgium)
The Humain Radioastronomy station (05° 15 12 E, 50°11 31 N), is located about 120 km to the South East of Brussels in the Belgian Ardennes.
A 6-m dish radio telescope is operated automatically and tracks the Sun from 7:30 till 16:00 UT every day.
Two spectrographs are currently installed, one is a Callisto spectrograph from the e-Callisto network. It covers the band 45 - 447 MHz. The other one, named HSRS is a SDR-based instrument used as a spectrograph. It covers the band 275 - 1495 MHz. The Callisto spectrograph is connected to a log-periodic antenna mounted as piggy bag on the side of the dish. The HSRS instrument is connected to a log-periodic antenna placed at the focus of the parabolic dish.
The instruments characteristics are the following :

Callisto HSRS
Frequency range 45 - 447 MHz 275 - 1495 MHz
Frequency resolution 63 kHz 98 kHz
Number of points in frequency 200 12500
Time resolution 0.25 s 0.25 s

Website

Solar radio spectrometer of Yunnan Observatories

Renaud Romagnan — 2018-07-12T09:25:54Z

Contact person : G. Gao

The metric solar radio spectrometer is located in Fuxian Solar Observatory (102°.57 E, 24°.34 N) of Yunnan Observatories (YNAO). The spectrometer includes a 11-meter meshed parabolic antenna and a digital FFT spectrometer . The working frequency range is 70-700 MHz (see Gao et al. 2014).

Parameters of YNAO metric spectrometer

Frequency range : 70-700 MHz
Antenna : 11-m meshed parabolic
Highest spectral resolution : 200 kHz
Time cadence : 80ms
Dynamic range : 72 dB (Maximum)
Recording time : 00:00-10:00 UT
Sensitivity : 1 SFU
Polarization mode : left and right circular polarization

SWAVES

Renaud Romagnan — 2018-07-12T09:25:12Z

SWAVES The Radio and Plasma Wave Investigation on the STEREO mission ( for a detailed description see Bougeret et al., 2008)

http://swaves.gsfc.nasa.gov/
Contact persons : M. Maksimovic, R. MacDowall

The SWAVES experiment includes the following instruments and components : (1) Radio receivers (HFR and LFRhi) that measure radio wave intensity, source direction, and angular size in the frequency range of 16 MHz to 40 kHz, corresponding to source distances of about 1 RS to 1 AU. (2) Low Frequency Receivers (LFRlo) that make sensitive measurements of radio and plasma waves near the electron plasma frequency at 1 AU (10-40 kHz). (3) A Fixed Frequency Receiver (FFR) that measures radio emissions at 50 MHz, at high time resolution, to complement ground-based radioheliograph measurements. (4) Time Domain Samplers (TDS) that simultaneously make wideband waveform measurements on 3 electric at one of several commandable sample rates and bandwidths.
Antenna systems include three mutually orthogonal 6-meter monopoles on each STEREO spacecraft. A Data Processing Unit (DPU) on each spacecraft controls and coordinates the various instrument components and performs digital signal processing.

The web page includes the data from one band of the LFR (40 kHz to 160 kHz) and the whole range of HFR (125 kHz to 16 MHz).

The following table summarizes the main characteristics of the concerned receivers.

Band C from LFR HFR
Frequency coverage 40 kHz - 160kHz 125kHz - 16.025 MHz
Bandwidth 2-octave 25kHz
Frequency resolution ΔF/Fo = 8.66% >=< 50kHz
Sensitivity 6nV/rootHz 6nV/rootHz
Dynamic range 120dB 80dB

J.L. Bougeret, K. Goetz, M.L. Kaiser et al. The radio and plasma wave investigation on the STEREO mission,Space Science Reviews, Vol 136, issue 1-4, 2008

WAVES

Renaud Romagnan — 2018-07-12T09:24:23Z

WAVES The Radio and Plasma Wave Investigation on the WIND Spacecraft (for a detailed description see Bougeret et al., 1995)

http://www-lep.gsfc.nasa.gov/waves/waves.html
Contact persons : M. Maksimovic, R. MacDowall

The WAVES instrument is a joint effort of the Paris-Meudon Observatory, the University of Minnesota, and the Goddard Space Flight Center (NASA).
The sensors are : (1) three electric dipolar antenna systems supplied by Fairchild Space (two are coplanar, orthogonal wire dipole antennas in the spin-plane, the other a rigid spin-axis dipole) and (2) three magnetic search coils mounted orthogonally (designed and built by the University of Iowa). After preamplification, the sensor outputs are routed to the analysis electronics, consisting in a low frequency (DC - 10 kHz) FFT receiver, a broadband (4 kHz - 256 kHz) multi-channel analyzer designed principally to study the electron thermal noise, two dual radio receivers covering the band 20 kHz to 13.825 MHz, and a time-domain waveform sampler (sampling to 120,000/s). The experiment is controlled by a central microprocessor (DPU) which can be used in flight to reconfigure the sensor outputs and to maximize the science return for the bit rate and power allotments that are available. A DC/DC power converter is also part of the electronics stack.

The web page includes the data from the two Radio Receivers RAD1 and RAD2 whose the characteristics are the following ones :

– Band 1 (RAD1) Inputs : Ex+Ez, Ez Frequency range : 20 kHz - 1,040 kHz No. channels : 256 Bandwidth:3 kHz Sensitivity : 7 nV/Sqrt(Hz)
– Band 2 (RAD2) Inputs : Ey+Ez, Ez Frequency range : 1.075 MHz - 13.825 MHz No. channels : 256 Bandwidth : 20 kHz Sensitivity : 7 nV/Sqrt(Hz)

Bougeret, J.-L.,M. L. Kaiser, P.J. Kellog et al., WAVES : the radio and Plasma Wave Investigation, Space SCi. Rev., 71, 5, 1995

Nancay Decameter Array

Renaud Romagnan — 2018-07-12T09:22:57Z

Nancay Decameter Array operated by the Observatoire de Paris and funded by the French research agency CNRS/INSU. (for a detailed description, see A. Lecacheux, 2000)

http://www.obs-nancay.fr

Contact person : contact_nda@obs-nancay.fr

The DAM, located at longitude 2 degrees east, latitude 47 north, operating in the 10-80 MHz frequency range, consists in two phased antenna arrays in opposite senses of circular polarisation with a 4000 m2 effective aperture each, and a set of receivers allowing for wide band, high resolution and sensitive spectroscopy of Jovian and solar radio emissions. Each array includes 72 antenna.

A. Lecacheux Radio Astronomy at Long Wavelengths, tutorials and reviews from an AGU Chapman conference held Oct. 1998 in Paris, France. Geophysical monograph Series, Vol. 119. ISSN 0065-8448. Edited by R.G. Stone, K.W. Weiler, M.L. Goldstein, and J.-L. Bougerot. Washington, DC : American Geophysical Union, 2000., p.321

ARTEMIS IV Multichannel solar radiospectrograph

Renaud Romagnan — 2018-07-12T09:20:14Z

ARTEMIS IV Multichannel solar radiospectrograph operated by the University of Athens, located at Thermopyle Satellite Station, Greece (for a complete description, see Caroubalos et al., 2001)

http://artemis-iv.phys.uoa.gr/
Contact persons : For ARTEMIS Spectra : P. Preka-Papadema or Alexander Hillaris or Xenophon Moussas
Scientific team : Xenophon Moussas, Costas Caroubalos, Giota Preka-Papadema, Athanasios Kontogeorgos, Panagiotis Tsitsipis, Alexander Hillaris
Costas Alissandrakis

ARTEMIS is located at longitude 22. 41 degrees east, latitude 38.47 north. Observations cover the frequency range from 20 to 650 MHz. The spectrograph has a 7-meter steerable parabolic antenna for 110 to 650 MHz and a fixed antenna for the 20 to 110 MHz. There are two receivers operating in parallel, one sweep frequency for the whole range (10 spectrums/sec, 630 channels/spectrum) and one acousto-optical receiver for the range 270 to 470 MHz (100 spectrums/sec, 128 channels/spectrum). The data acquisition system consists in two PCs (equipped with 12 bit, 225 ksamples/sec DAC, one for every receiver) ,Windows operating system, connected through Ethernet. The daily operation is fully automated : pointing the antenna to the sun, starting and stopping the observations at preset times, data acquisition, and archiving on DVD. The whole system can be remotely controled.

C. Caroubalos, D. Maroulis, N. Patavalis, J-L. Bougeret, G. Dumas, C. Perche, C. Alissandrakis, A. Hillaris, X. Moussas, P. Preka-Papadema, A. Kontogeorgos, P. Tsitsipis, G. Kanellakis. : The New Multichannel Radio spectrograph ARTEMIS-IV/HECATE, of the University of Athens. Experimental Astronomy 11 : 23-32, 2001.