Absorption in Solar Atmosphere
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1 Absorpto Solar Atmosphere A black body spectrum emtted from solar surface causes exctato processes o atoms the solar atmosphere. Ths tur causes absorpto of characterstc wavelegths correspodg to those atoms that are the most abudat oes the solar atmosphere absorpto spectroscopy.
2 Solar mttace Spectrum ultravolet frared vsble c 1 1 Waveumber: k cm Spectrum s characterzed by may atomc absorpto les, prmarly by H-Balmer seres of hghly abudat hydroge.
![The Hydroge Atom http://www.walter-fedt.de/ph14e/bohrh.htm http://www.falstad.com/qmatom/ = l=1 Z ev 136. s eergy ecessary to oze atom Z s charge of ucleus, Z = 1 9 r 59. 1 [ m] 1366.](/docs-images/81/84025014/images/3-0.jpg "[ ev ] = l= =1 l= : ma quatum umber, =, 1,,... l : orbtal mometum quatum umber, l = 1,, 3,...-1 m: magetc quatum umber, l+1 values from -l, -l+1.")
3 The Hydroge Atom = l=1 Z ev 136. s eergy ecessary to oze atom Z s charge of ucleus, Z = 1 9 r [ m] [ ev ] = l= =1 l= : ma quatum umber, =, 1,,... l : orbtal mometum quatum umber, l = 1,, 3,...-1 m: magetc quatum umber, l+1 values from -l, -l+1... l+1, l s = ½ sp quatum umber, s=1/, -1/ lectro trasto betwee orbts requres or releases eergy:
4 Trasto betwee ergy Orbtals Possble emsso or absorpto of lght wth fxed wavelegths by trastos of electros betwee orbts! Wavelegth depeds o eergy dfferece betwee orbts! Hydroge emsso spectrum Balmer Seres N=3 H α : =656.3m = -13.6/ N=1, shell N=, L shell =1 N=3, L shell L trastos = N=4, N shell
5 ergy ad Wavelegth of emtted or absorbed Photos f f h c h 1 1 h c f ev ev 34 h Plack Co stat: [ J s ] c Speed of L ght: 13.6 ev c h [ m / s ] 1 m R H
6 Mult-lectro Atoms Z s the charge ad determes the chemcal characterstcs of the elemet, e.g. Z=1(Hydroge, Z= (Helum Z=8 (Oxyge. lectro trastos ad photo emsso s more complex ad depeds o Z ad the sheldg S by er electro shells. -trastos to =1 Z S Z 1 Z hc hc Z 1 Z hc
7 Z eV He: Z L L xample: Calculate the ad L UV-Ray Les for He ev 1 1.eV ev 1 1.9eV Z eV h c h c 1.6m α ev 1.889eV 656.8m h c L 11.6m β L α =3 = =1 α ad trastos the ultravolet rage! L α ad other L ad M trastos vsble rage
8 Characterstc Spectrum of lemets Solar Spectrum ach elemet has ts ow characterstc trastos depedg o the orbt quatum umbers ad the charge Z (umber of electros, protos. These trastos ca be aalyzed by spectroscopy of the lght to determe the elemetal abudace! ultravolet vsble frared
9 Absorpto the arth Atmosphere Absorpto ad scatterg of radato the atmosphere depeds o the chemcal ad physcal composto of the atmospherc layers. Ths cludes dust ad molecular composto, mosture, temperature as well as desty. It also depeds o the ature of the teracto processes of the comg (ad extg radato (photos wth the atomc ad molecular gas compoets!
10 Solar Radato Atmosphere I I ( e d ( e (, x dx ( trasmtted radato (,x absorpto coeffcet x: thckess of atmosphere layer The absorpto coeffcet cludes absorpto probabltes by molecular rotatoal or vbratoal exctato processes, ad photo scatterg, t depeds o the composto of the atmosphere ad ts atomc ad molecular compoets: N, O, O 3, CO, CH 4, H O
11 Absorpto Probabltes Trasmsso ( (, x dx ( e (, x ( x x The partcle desty (x depeds o the overall radal desty depedece ad the mass fractos of the gas compoets the dfferet atmospherc layers. X ( x A N A Absorpto (heat producto absorbg materal x dx abs( ( (, 1 (x: partcle desty (cm -3 (: cross secto (cm 1 ( e The cross secto s the teracto probablty of lght (photos wth a certa wavelegth or eergy =h wth varous atmospherc gases ad dust partcles (exctato ad scatterg
12 Atmospherc Composto
13 Physcal ad Chemcal Characterstcs Ar mass fracto Large varato (x wth alttude for dfferet gaseous elemets ad molecules I. rchmet of H O vapor lower atmosphere, the troposphere. CO, O, Ar farly cotuous, O 3 break up stratosphere!
14 Raylegh Scatterg Raylegh scatterg s the elastc scatterg of lght by partcles of sze d much smaller tha the wavelegth of the lght, such as molecules or dust partcles. Raylegh scatterg s a fucto of the electrc polarzablty of the partcles. d d 1 m ( Volume polarzablty: gas = cm 3 Scatterg cross secto creases wth lower wavelegths, blue lght gets more scattered tha red lght. It gves the sky ts typcally blue color (otherwse sky would have solar whte spectrum color. Lookg at suset, scatter has creased because of creased thckess of atmospherc layer, blue s removed from le of sght to su. blue red
15 xample Calculate Raylegh scatterg cross secto o ar for blue b =45 m ad red lght r =65 m; gas = cm 3 ( cm 44 4 ( ( ( ( b b r cm 9.64 mbar 7.1 cm. mbar 1bar 1 4 cm
![A N A x X x x x ( (, ( 1 1 1.11, ( 4 1 9.1, ( 1 3.33 ( ( 1 1.3 ( ( 5 6 5 5 e e e e e e d dx x H d dx x ar x α A [cm -3 ] σ [cm ] cm 1 N.78 1.77 8 1.6776+ 4.67145-7 7.8366-5 O.19.8 3 3.5756+1 9.](/docs-images/81/84025014/images/16-0.jpg "543-8 3.41-6 Ar.1 1.66 38 1.5847+ 4.1886-7 6.5115-7 H O.1 1.48 18 3.3456+ 3.669-7 1.97-6 CO.3.63 44 4.159+19 1.3137-6 4.347-7 SO 4.1 4.34 98 6.1449+18.8856-6 1.758-7 Ar.994 1.7.891+ 4.396-7 9.")
16 A N A x X x x x ( (, ( , ( , ( ( ( ( ( e e e e e e d dx x H d dx x ar x α A [cm -3 ] σ [cm ] cm 1 N O Ar H O CO SO Ar everythg scattered 66% scattered Wave legth =55 m, Desty 1g/cm 3, Thckess of atmosphere layer d1 km
17 σ( [bar], T( Raylegh Scatterg Scatterg cross secto bar Trasmsso through 1 km ar (vertcally 5 4 ( k 44.7 k / red blue ( x dx e (, ( ar e d [m] Trasmsso through 3 km ar (horzotally Wave umber k=1/ [cm -1 ]
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