Secchirh

SolO surveys

Renaud Romagnan — 2022-05-30T08:42:28Z

The composite survey SolO 8h covers the 08-16 UT time range (1pixel/60sec) and zooms are 1 hour long (1pixel/10sec).
The composite survey SolO 24h covers the 00-24 UT time range (1pixel/180sec) and zooms are 3 hours long (1pixel/22.5sec).

It is composed of

EPD : the time histories of protons and electrons (A).
a spectrum (B)
NRH : a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time at 150 MHz (C)
STIX : the count time histories (D)

EPD : The time histories of protons and electrons (A)

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.

Multi-instrument spectrum (B)

Frequency range 600 MHz-20 kHz. Logarithmic scale.
Combines data obtained with :

Instrument	Fmin	Fmax	Time resolution
Waves RAD1	20 KHz	1 MHz	1 min
Waves RAD2	1.04 MHz	13.8 MHz	16 sec
NDA	20 MHz	70 MHz	1 sec
ORFEES	144 MHz	1000 MHz	1 sec

NRH : EW and NS brightness distribution versus time at 150 MHz (C)

Integration time : 10s (1 point/ 60s)
Each frame contains a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time ; the units of the vertical axis are solar radius.

STIX : The count time histories (D)

the count time histories in 20s time intervals in three photon energy channels (4-10, 10-15, 15-25 keV).

ORFEES Real Time

Renaud Romagnan — 2018-10-23T07:02:48Z

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High Resolution Image

Renaud Romagnan — 2018-07-23T08:47:00Z

You can view here Rotational synthesis images.

Their advantages, when compared to snapshot images, are :

A better sensitivity and a strong reduction of interferences, both resulting from the long observation time.
A better spatial resolution (respectively about 3 and 2 times better in the EW and NS directions) and a field of view wider by a factor 1.5 in the EW direction, due to a much more complete uv-coverage.

The dynamical range in images of the quiet corona is much larger than in snapshot images, with a sensitivity of a few kK and a mean accuracy of 15 kK. The counterpart is that the sun must be quiet, or with a low-level time-varying activity, which excludes active days.

You can download PDF yearly quicklook.

Spectral 00h to 08h UT SURVEY

Renaud Romagnan — 2018-07-02T14:27:42Z

The Spectral 00h to 08h UT SURVEY covers the 00-08 UT time range (?pixel/ ???sec) and zooms are 1 hours long (?pixel/ ???sec).

It is composed of :
a spectrum (A)

Multi-instrument Spectrum (A)

Frequency range 0.02 MHz kHz. Logarithmic scale.
Combines data obtained with :


Instrument	Fmin	Fmax	Time resolution
Waves RAD1	20 KHz	1 MHz	1 min
Waves RAD2	1.04 MHz	13.8 MHz	16 sec
Culgoora	25 MHz	100 MHz	? sec
Ynao	100 MHz	700 MHz	? sec
GLOSS	40 MHz	440 MHz	250 msec

Note : Sometimes, Learmonth is used also for the frequency range from 25 MHz to 100 MHz instead of Culgoora.

STEREO/SWAVES and WIND/WAVES 24h SURVEY

Renaud Romagnan — 2018-07-02T14:26:33Z

The STEREO/SWAVES and WIND/WAVES 24h SURVEY covers the 00-24 UT time range (1pixel/180sec) and zooms are 3 hours long (1pixel/22.5sec).

It is composed of :

three spectra from spatials data (A,B and C)
a position of CMEs detected by STEREO A and B layered over the spectra (Red and blue triangles)
a position of CMEs detected by SOHO in a 24 hours time range (D)

It is available from the STEREO launch on october 2006.

3 spectra

Logarithmic frequency axis.

1) STEREO WAVES A (A)

2) STEREO WAVES B (B)

The spectra from SWAVES A and SWAVES B are placed head to tail.

STEREO A and B spectrum
Instrument	Fmin	Fmax	Time resolution
SWAVES LFR	0.04 MHz	0.160 MHz	between 15s and 30s
SWAVES HFR	0.125 MHz	16.025 MHz	between 15s and 30s

3) WIND/WAVES (C)


Instrument	Fmin	Fmax	Time resolution
Waves RAD1	20 KHz	1 MHz	1 min
Waves RAD2	1.04 MHz	13.8 MHz	16 sec

Coronal Mass Ejections (CMEs) form LASCO (same as Composite I survey but in a 24h time range)

STEREO LASCO CMEs (D)

Time of appearance in SOHO/LASCO C2 and direction (arrow)
Speed V(First order, km/sec), angular width W(deg)
Black : detected in C2 and C3
Grey : detected in C2 only

STEREO CMEs (Red and blue triangles)

Time of appearance in STEREO A (red triangle) and STEREO B (blue triangle)

Composite 2

Renaud Romagnan — 2018-07-02T14:18:48Z

The COMPOSITES SURVEYS IIa and IIb covers the 08-16 UT time range (1pixel/60sec) and zooms are 1 hour long (1pixel/10sec).

IIa

IIb

These two surveys are similars except for the EW and NS brightness distributions versus time (C and D) which is :

greyscale (same as COMPOSITE I) for the COMPOSITE IIa
contour plot for the COMPOSITE IIb

The two spectra (A and B) reported in these two surveys are similars .

They are composed of

two spectra (A and B)
two displays of brightness distribution projected onto the heliocentric East/West or North/South direction versus time at 150/164MHz (C) and 432MHz (D)
a position of CMEs detected by SOHO (E)

Two Spectra

1) from 10 (or 20) MHz to 70 MHz. Linear scale.(A)

This spectrum displays data from DAM. When DAM is unavailable, Artemis is used instead.


Instrument	Fmin	Fmax	Time resolution	Dates
DAM	20 MHz	70 MHz	1 sec	From 1st Jan 2002 to present
Artemis	20 MHz	70 MHz	5 sec	From 1st Jan 2002 to present

2) from 100 MHz to 2000 or 600 MHz. Linear scale.(B)

This spectrum displays data from Phoenix 2 because of his frequency range (which goes to 2Ghz).
When Phoenix 2 is unavailable, Artemis is used instead up to 600Mhz.
Please note that Phoenix 2 is no longer operationnal from 16 march 2009. So after this date, Artemis is systematicaly used.


Instrument	Fmin	Fmax	Time resolution	Dates
Artemis	100 MHz	600 MHz	5 secs	From 1st Jan 2002 to present
Phoenix 2	112 MHz	2000 MHz	1 sec	From 1st Jan 2002 to 16 march 2009

EW and NS brightness distributions versus time at two frequencies

150 MHz (164 MHz before 01 Dec 2006) (C)
432 MHz (D)
Each frame contains a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time ; the units of the vertical axis are solar radius.

IIa displays in greyscale : each scan is normalised to its maximum. All the bursts are visibles but the intensity variations during the day are not well described.
IIb displays in contour plot : the normalisation is made on the maximum intensity in the whole day. Contour levels are chosen in order to describe the quiet sun (at least one level) and intenses bursts. This gives a good estimate of intensity variation with the day.

NRH Projection Resolution Time
Survey	Integration Time
IIa 8h-16h	120s
IIa zoom	10s
IIb 8h-16h	60s
IIb zoom	10s

Coronal Mass Ejections (CMEs) (E)(same as Composite I survey)

The CMEs are reported in the composites IIa and IIb survey from 08 to 16 UT.

Time of appearance in SOHO/LASCO C2 and direction (arrow)
Speed V(First order, km/sec), angular width W(deg)
Black : detected in C2 and C3
Grey : detected in C2 only

Composite 1

Renaud Romagnan — 2018-07-02T13:59:07Z

The COMPOSITE SURVEY I covers the 08-16 UT time range (1pixel/60sec) and zooms are 1 hour long (1pixel/10sec).

It is composed of

a spectrum (A)
a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time at 150/164MHz (B)
a position of CMEs detected by SOHO (C)

Multi-instrument Spectrum (A)

Frequency range 600 MHz-20 kHz. Logarithmic scale.
Combines data obtained with :

Instruments_composite1
Instruments used in Composite I survey
Instrument	Fmin	Fmax	Time resolution	date
Waves RAD1	20 KHz	1 MHz	1 min
Waves RAD2	1.04 MHz	13.8 MHz	16 sec
DAM	20 MHz	70 MHz	1 sec
Artemis	70 MHz	600 MHz	5 sec	Until 01 nov 2012
ORFEES	70 MHz	1000 MHz	1 sec	Since 01 nov 2012
Humain Callisto	45 MHz	447 MHz	0.25 sec	Since 01 July 2016
Humain ARCAS	45 MHz	450 MHz	84 msec	Since 01 Jan 2017
Humain HSRS	275 MHz	1495 MHz	0.25 sec	Since 15 oct 2015

Note : When DAM is unavailable, Artemis is used also for the frequency range from 20 MHz to 70 MHz or Humain since 1st july 2016.

EW and NS brightness distribution versus time (B)

150 MHz (164 MHz before 01 Dec 2006)

Integration time : 10s (1 point/ 60s)
Each frame contains a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time ; the units of the vertical axis are solar radius.

Coronal Mass Ejections (CMEs) (C)

The CMEs are reported in the composite1 survey from 08 to 16 UT.

Time of appearance in SOHO/LASCO C2 and direction (arrow)
Speed V(First order, km/sec), angular width W(deg)
Black : detected in C2 and C3
Grey : detected in C2 only

Plots-Movies

Florence HENRY — 2017-05-23T08:56:08Z

If you use data from this survey, we would appreciate an acknowledgment as follows :

"We thank the radio monitoring service at LESIA (Observatoire de Paris) to provide value-added data that have been used for this study. "

We also ask an electronic copy of any publication that acknowledges the survey.

"Please add a similar acknowledgement for all instruments used for the composite spectrum, for example, "We are grateful to -name of the instrument's institution- for giving access to the data to produce the composite spectrum"

First and last available days

Composites: First : 01 January 1997; Last : 30 May 2026
24h Waves/Swaves: First : 01 January 1997; Last : 28 May 2026
Spectral UT 00h->08h: First : 01 January 1970; Last : 28 May 2026
SolO: First : 01 January 1970; Last : 24 May 2026

NRH Real Time

Florence HENRY — 2017-05-22T21:01:07Z

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