English                             To main page of CrAO         Solar service "KRIM"                                  

    Eng  | Rus

News

About

Observations

Telescopes

staff

Conferences

Publications

Links

 


On this page:

  Solar Mean magnetic field (MMF)
  HeI 1083nm solar images
  H-alpha solar images

Sunspots:
         
Sunspots magnetic fields
         Synoptic maps
         Daily relative sunspot numbers


Observation method
MMF obtaining with the aid of the
telescope TST-1 of the Crimean Astrophysical Observatory.
The archive of MMF data is here.

Latest MMF data

Observation method
The solar images in the HeI 1083nm line are obtaining with the aid of the
telescope TST-2 of the Crimean Astrophysical Observatory. They are obtained due scan toning of the Sun images through the slit of the spectrograph. The photometer detects the intensity in the center of the HeI 1083nm line. The telescope and detecting device are served by PC/AT 386 computer. The time of observation and space resolution ix, iy are given in the observation list. All images presented at the page are normalized to 9.8x9.8 arc sec per pixel. The equator direction is approximately horizontal. Right images are corrected for limb darkening and left ones are not corrected.
The archive of images in the HeI 1083nm line is here.

Latest.gif (58291 bytes)
Latest image

Observation method
The coronagraph-1 (KG-1) was designed by the State Optical and Mechanical Plant according to the Lyot layout and put into operation in 1951. Positioned on the equatorial mounting, it is a refractor with the 21-cm objective. The objective is made of glass K8. It is a convex-plane lens 10 mm thick with the 350-cm focal length in the H-alpha 6562.8 line. The telescope is used for chromospheric monochromatic observations of prominences, filaments, active regions and flares in the H-alpha line. In the focal plane of the objective there is a diaphragm cutting out a part of the solar image. Next to the diaphragm there is another objective. Passing through it, a beam becomes parallel. Then light falls on the diagonal mirror and interference-polarization filter (IPF). After IPF light goes to the diagonal mirror, then to the lens of the field, and depending on the rotary motion of the third diagonal mirror, either to the ocular or to the digital camera. The focal length of this layout is 7 meters. The 12-cm image of the Sun is built up in the focal plane. Optical resolution of the telescope is 1.5”.

Attached equipment
1 Interference-polarization filter Halle. The passband is 0.5 - 1 , a shift to wings up to 1 is allowed. The temperature of IPF is controlled by a thermostat; working temperature is 40.7 ?.
2 Digital camera Canon EOS 1000D, reflex camera with a portable objective, 10.50 million pixels, matrix: 22.2 x 14.8 mm.

Observations
An image of a part of the solar disk (3888 2592 pixels or 355.5 266.6 angular seconds in size) is taken with the digital camera. The image is oriented across the diurnal circle. Observations are carried out in the center and in wings of the H-alpha active regions and filaments on the solar disk, as well as prominences on the limb.


The archive of images in the H-alpha line is here.

Send notes and request to Shakhovskaya A.N. anna@craocrimea.ru

latest.jpg (30362 bytes)
Latest image

Observation method
Visual measurements of sunspot magnetic fields are carrying out in the
Crimean Astrophysical Observatory from 1955. First two years the line FeI 6173 A was used. Since 1957 observations are carrying out in the line FeI 6302 A. Maximal distance between sigma-components is measured in the profile of this line splitted in a sunspot magnetic field. Then the measured size is transferred in intensity of a magnetic field.
The data of observations of each day are presented in a kind of sketch of the solar disk with all sunspot groups and their temporary numbers. Near each sunspot the sign of magnetic field ( N or S) and intensity in hundreds Gauss is specified. The moment of observation (UT), quality of the image (seeing) in five step scale and scintillation (Scintillation) in arc seconds is specified above the sketch. The line EW corresponds to a direction of an equator.
The archive of sunspot magnetic fields is here.

Latest.gif (15884 bytes)

Latest map


              

 

Observation method

The synoptic maps are built on observation data obtained at the
Tower Solar Telescope BST-2 of the Crimean Astrophysical Observatory.

These data involve areas of sunspot groups and intensity distribution of the HeI 1083 nm line across the solar surface for each rotation of the Sun.
The areas of sunspot groups are detected based on sketches in white light of the 110-mm-diameter Sun's disk.
The HeI line intensity is determined by scanning the solar disk with a multi-purpose spectrophotometer.
The maps being built taking into account solar limb darkening and normalized to a unit are filled with isophotes 0.9 typical for brightness in active regions and filaments and 1.02 typical for coronal holes.
The region defined by isophote 0.9 is marked in yellow and defined by isophote 1.02 - in brown.

The position of sunspot groups for each observation day is indicated on the synoptic maps. The area of a group is represented by a rectangle, lengths of sides are equal to longitudinal and latitudinal                                   
extension of the sunspot group. Individual sunspots are represented by dots.

Two vertical dashed lines correspond to the starting and ending
of the Carrington rotation. Dashes directed downward along the x axis
indicate longitudes of the central meridian (Lo) in moments of observations.
The archive of synoptic maps is here.

Send notes and request to Perebeynos V.A. schana@craocrimea.ru      

 

 

 

 

 

 

 

Latest map

                                                                

                                                                                                                                                                                               

 

observations_htm_wolf.gif (1159 bytes)

Observation method

The daily relative numbers of sunspots (Wolf number) are the basic index of solar activity. Daily index of sunspots activity R, defined as R="k" (10 g + s), where S the number of separate sunspots, g number groups of sunspots are k-th the normalizing factor, which considers difference in the sensitivity of the utilized tools and which leads the observed values to the standard Zurich numbers.

k=1 for CrAO measurements.
The central zone of Sun is not included in the total amount of R = k (10 g + s) for the Sun (full).

Wolf numbers data -txt files (RNmmyy.htm),
where mm-month, yy-year in the form of tables (columns from left to right):
Day, hhmm-Universal Time (UT), s-quality visible image on a five-step scale (Seeing),
Ngr-number groups of sunspots, Nsp-the number of separate sunspots, W-daily index of sunspots activity R (full-total Sun,
in N-hemisphere-northern hemisphere, in S-hemisphere-southern hemisphere, in central zone-central zone of Sun)

Latest data



Send notes and request to Borisenko A.V. wildkr@craocrimea.ru

Daily relative sunspot numbers click here

 

news | about | observations | telescopes | staff | conferences | publications | links

Solar Physics Laboratory, Crimean Astrophysical Observatory, 298409, Nauchny, Crimea, Russia
-

Head of Solar Physics Laboratory - Lead. sci. Valentina I. Abramenko
-

I