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THE PROBE LAYER METHOD IN THE CALCULATIONS OF CONTRIBUTION AND RESPONSE FUNCTIONS S.G.Mozharovsky
Ussuriysk Astrophysical Observatory of FEB RAS, Ussuriysk, Russia sw@newmail.ru The method of probe layer for the calculation of response and contribution functions is discussed. The method is based on a numerical calculation of the formation of spectral line profiles. Calculating the profile of the line in the usual way, we can change a physical parameter in a narrow layer of the photosphere and calculate profile again. Consistently moving probe layer over the entire depth of the photosphere, and each time calculating the difference between the original and the changed profiles we can get the distribution of response to a perturbation with height. In this work it is shown that the perturbation must be chosen with care. Thus, incorrect choice of Wittmann [2] led him to the wrong conclusion, that there is great uncertainty in determining the depth that generate the observed value of the magnetic field. We have proposed in the probe layer to equate to zero the coefficients of the ratio of selective and continuous absorption in line center 0 . This allows us to turn from the response functions to the contribution functions calculated with help of the probe layer (CFPL). CFPL are easy to understand, they take into account all the processes of emission and absorption in line formation, energy exchange between Stokes parameters intensity etc. Thus, such contribution functions are close to ideal and perhaps deserve greater use.

(CF) . , , . , , , , . , (. .[1]). , , . " ". (RF) (1974) [2], (1972) [3], .


RF , . - , .. - " " , . . , . . , , , . . , ­ 2000 0 , - 0.5 lg ( ) . V- VMAX . , :

.1. lg ( ) ~ 0.5 . lg ( ) = 0.1 0.05 VMAX .

, , , RF, . , 6173 0 2000 :


2100 ,

- . 2000 RF :

.2. CFPL lg ( ) = 0.1 0.05 V- VMAX V- WV .

, VMAX ­ , . WV - V. ­ 0 . , , . . [4]. , . . , , , . , 0 , . , , , . , . D - D* , X = lg ( ) , CFD , x = ( D - Dx* ) / D . W - W * , h () CFW ,h = (W - Wh* ) / W .


. , , , lg ( ) h . , , [5] , :

.3. - ( ) Fe I 5250 A HOLMU+VAL HOLMU VAL .

CF, , CFPL [6]:

. 4. ( SunWorld) Fe I 5250 A HOLMU Chapmen.

, , , . , , , :
CF 0 S
Gurtovenko E.A., Sheminova V.A., Sarychev A.P. // 1991. Solar Phys., v.136, p.239-250. Wittmann A. // 1974. Solar Phys., v.35, p.11-29. Staude J. // 1972. Solar Phys., v.24, p255-261. Grigoryeva S.A., Turova I.P., Teplitskaja R.B. // 1991. Solar Phys., v.135, p1-14. Grossmann-Doerth U., Larsson B., Solanki S.K. // 1988. Astron. Astrophys. v.204, p.266274 6. Almeida J.S. // 1992. Solar Phys., v.137, p.1-14

1. 2. 3. 4. 5.