{ 54 1 { 1 � � 8 } � Vol.54 No.12013 � 1 ; ACTA ASTRONOMICA SINICA Jan., 2013

� K�`4iI*B5e&��∗rnl 1 x s 1 tpm 1† j w 2 oqk 2 yuv 2

(1 <�℄�e�AI*~�mH�8 C| 650500)(2 jK:�8<��9� C| 650011)a^ ���P~G<K (Solar Dynamics Observatory, SDO) x?u��d�E℄J# (Atmospheric Imaging Assembly, AIA) �O 3 5y�+/Æ (171 A�193 A W

211 A) uG<|[JQY��m�. (AR 11092) Mqug.Gu=�U,�On/�Qb�"^B&m�.ug�-=�U,�4&{Wug�P��U,�ug `�ugiG<pu=�U,��7�[1�d����0n 40∼121 km/s, �^�!#d&W��7 %�g��|g)rS `u%�dd�OVSnk/~o�0�u�ugu=�q�B2!/Æ (3 5y�+/Æ) o"{Ou.(��^B 3 min �| 10 �$luq��Z+�2��ug=�&QK 3 min Æ$uq��J)>u[�.-!^BV!uRlq��O5�M&{[�Rln<�SOJ)�|O�.paAuu�/7! P℄�HA�P℄�b#�P℄�hT-J�P℄�1(G��dR+<2� P182; WZ�M?� A

1 _\ ��B℄A%�� �htW`�O}.!jWV. �AWV.V��".w��hjWV.JPAx+�{tfh�Nm.tT+kn tfVx+�YQk)�� typ�t<���(�!?1�Nh.�Pa(��t ��>tfs UE��Y��(jWV.t<�T+m���H}tÆ4o�>���%��-7& SOHO (Solar and

Heliospheric Observatory)�TRACE (Transition Region and Coronal Explorer) V SDO t��� 20 yrD>ro2X U!EjWV.AtfVx+h<�T+tN��Ofmanw [1] u[�N SOHO �H\z,�Px+h�.t℄A�1)� DeForest w [2] �SOHO/EIT F;ox+hQ{yp��.t℄A� Ofman w [3] ?1Nm<�mjWV.�De Moortelw [4] A TRACE/171 A. h F;oXtfhF�t<�T+t℄A�Ær ?1NmQktT+mjWV.� Robbrecht w [5] A��XtfA 171 AV 195 A S4. t<�T+'Ba�?1aM��MT+��:A�aD��z SDOZ?�0a�?�# etF;{ZiX>r���"K�?�w�(tv�� 2011

2012-02-20 tq22� 2012-06-13 tqu/2∗ K��;:�s�[� (10878014, 11063005) X<�\�;:�s�[� (2009CD046, 2007A194M) }v† lhf@ynao.ac.cn

28 � 9 � � 54 1�� Krishna Prasadw [6] �N SDO/AIA tF;�Px-+�Vx+�℄A 10∼30 mintyp�<��Nh<�tT+���/m 100∼170 km/s.Y*�i!y�!E��Z�tjWV."��(�De Moortelw [7] �zX 384Lptf<�j���PNh<�T+Pa#B4%Z�-,��_��� (25∼165 km/s)�LpWAT+����Q)(�$����B % 12%. 8, De Moortel w [7−9] tyx��p�ttf<�T+�B�Y%Z�O��Cp�tG(��Z�?E�y��(M?1 3 min tZ���QkV 5 min t P }QkT+;��NI(�{N-o`y�t [10−14]. _*� ! UtCp�t�tQkF;�hm��1`NhQkt3Q1&N� �D�E%tf<�T+htj.(�g`t=� �gX℄��h��in!�g��Y�"9;�tf<�p�{�T+��m℄o�t;���;�.���1�9�t�ttg{THIz�1z℄}�V�t�>Hg}n�>o�tj �,V�X{Z [15]. >rA�8h���tm� SDO/AIA x~*. 171 A � 193 A V 211 AF;otZ�O�tf|OQk�tft<�A1 6�MtT+�T�{��NmQkt;�w�3�2 0�3N:�=.��(��m ';tf<�T+t��� .#C;tft��Qkp��AIA � SDO �_>� SDO/AIA 1�w{��6�O 0.5 R⊙t�tVN-�>X0a�?�# etF;z,�,I"�A 7 4x~*. (Fe XVIII (94 A), Fe VIII �XXI (131 A), Fe IX (171 A), Fe XII �XXIV (193 A), Fe XIV (211 A), He II (304 A) V Fe

XVI (335 A)) aF;��t6�w\�?�# e1 1.5 arcsec, �A# �w"K�?�a�# e21 12 s, ;�5J�wl�.�t�d�T��;��6�wQ{ 24 h�sF;��A1�((��Z�!Ettf<�T+'B�>;9tz,�>r�'|24% AR 11092 l�-t|hA��Z�O�tLptf�1�(�a�,�(z,�2ta� m 2010 � 8 : 3 � 22:00 b 22:50. 6bo���w=��F;�#4d"9�FDt�Y�>r�,z,�X�?�w.U�l�- AR 11092 A>r�|ta �?������1<��1℄A Aschwandenw [16] F;ot^_tfQk�' 1(a) 7J,l�-�LptfA 171 A . t'\�\'h;5o�WARy+_p/�Httf��H3 (f) O℄V��zG|/GtH fsÆ���AQ{t 12 s pWt AIA/171 A � AIA/193 A V AIA/211 A }�h�>r5o1 . tfO�℄A℄�tQk��h 171 A . ���� 193 A V211 A U��F�� !�g`�WAR_*Tv�fMwm�H. F;ot��Z�- ((c) '�h), },fQk34%Z�O��tfQktT+;�(Z�!E�1 . tF;z,��X1 ttf(SpD6��1X�&N1 6�M<�Atf�_tT+'B�>r�tf�H�_�X 3 4x~*. (171 A � 193 A V 211 A)#'A 3 44dOta� '��|4d1 171 A . '\h�#ht slit1� slit2 V

1 � JP�x�lXX0C\�P!vhjvV- 29

slit3.

(a) AIA 171

60 80 100 120 140x / arcsec

60

80

100

120

140

y / a

rcse

c

slit2

slit1

slit3

(b) AIA 304

60 80 100 120 140x / arcsec

60

80

100

120

140

y / a

rcse

c

(c) AIA 1600

60 80 100 120 140x / arcsec

60

80

100

120

140

y / a

rcse

c

( 1 2010 � 8 ; 3 B 22:00 M� SDO/AIA psvn�/ 11092 Nr��C 171 A (a) � 304 A (b) X1 600 A (c) v(^ (a) (jxT (T 1 �T 2 XT 3) �2b�!�(v885eÆ (b) (v�K`� “+” $���Sm5

Fig. 1 The fan structure images of active region 11092 obtained by SDO/AIA in 171 A (a), 304 A (b),

and 1600 A (c) at 22:00UT on 2010 August 3. In panel (a), the reference position is used to compute the

space-time by three dashed lines (denoted by slit1, slit2, and slit3); In panel (b), the oscillation source of

the umbra is denoted by the white cross “+”.

3 L6FCS - ��O'171 A � 193 A V 211 A 3 4. ta� D' 2 �h�^r%ha��rm' 1(a) h#d'_a'tC� (^=�1 f).\' 2 h;�5o�tfA 3 41 6�M (T171≈0.8 MK � T193≈1.25 MK V

T211≈1.99 MK) �℄Az�U�t$i�:�Nh�:�T�Rz�PX��6�M<��tftT+'B��:A f-,℄zN��z(f/GtH sÆ�F��h 171 A . �:�T�C���06�t 211 A . �:�"1zN�Nh�:t���d)�m�$��t 4%∼6%. �:��O�a�!JdzJP�U℄�:Z�t�3mtf<�T+tp���$iH�f%tft<�T+$��� ��NNh�:;�B�JLptft<�T+����%;�℄Attft )�^_=�n t9�^B�ft��VqR1 U�w���a� 'h��Ptft<�T+��;�1`Æ4�>rNK2�:�f%ttn���1Tv���' 2 h�hiR�f%t��m>r�|2tp�a'MttnTv���>r;JtfA 171 A . t<�T+��U�_*S4. ��T+��A/| 5 arcsec �t℄_�����/m 59∼74 km/s; i.��,*T+a����℄&:H �:a�Æ_�℄�{T+\o/| 20 arcsec O���℄�/m 80∼121 km/s (D' 2(a)∼(c) �h). ( 171 A . 1 tm�tfh4% 193 A V 211 A S4. tT+��A/| 2 arcsec O� ��z��1<�t��T+�.tT+/G�����℄t�/#'m 46∼59 km/s V

30 � 9 � � 54 140∼58 km/s (D' 2(d)∼(i) �h). ��tfA 3 4. t.tT+�T�.A 193 A V211 A S4. h2JP���*"�T+/G���(�1��tfA06. T+��:C�|��Nm<�T+mÆmj. (06��M>Tnfe:0), �1m�g`�8,tf��Qk)�V��.!tT+���T�,<�T+;�mjWV.�tfhV�(6�!DMEIg Cs≈152 T

1/2 m·s−1, �h T tg41 K. �,,EIg� 171 A (0.8 MK) � 193 A (1.25 MK) V 211 A (1.99 MK) 3 4. AtfhtV�#'1 136 km/s � 170 km/s V 215 km/s. �%F;qRt1���;���Hg℄ �Robbrecht w [5] �oZ����2 %V��6b$�f��NURmj.}n�/�t�tf<�T+��A06. tF;��HgO�,�y6. �hm�L8U��Æ4;�t1�m 193 A V 211 A (StpD6�0�D�5ottf4%:0t=[�Nhft$�: �D$���:y�

V2=80 km/s

V1=74 km/s

V2=121 km/s

V1=59 km/s

V2=119 km/s

V1=69 km/s

V=51 km/s V=46 km/s V=59 km/s

V=40 km/s V=42 km/s V=58 km/s

( 2 ( 1 iv 3 �T5eQ%)C AIA 171 A � 193 A X 211 A 3 60�vb�!�( (W^). q6(j�;PvjT�EC�0vV-��}ÆxT�v/.3Æ3�'e0%DFig. 2 The space-time maps (running difference image) with time on X-axis, constructed from slits 1, 2,

and 3 (see Fig. 1), in three coronal channels of 171 A, 193 A, and 211 A, respectively. The slanted line

following the ridges, as marked in each panel, is used to estimate the propagation speed. The horizontal

dashed lines enclose the region averaged for the wavelet analysis.

1 � JP�x�lXX0C\�P!vhjvV- 311XX N 3 4. t��?��>r�2X 7 d a��Z�A�wE�atft9q' (D' 3 �h).�%Ca�t�d�tf?�3ID�tp��>ra��N���Lp-,9q'A 3 4. �V4#tL�DX tf4%�whka�$���t?��' 3 �h1tf4%��E�aA 171 A � 193 A V 211 A . 9q'�>r|2X 171 A . Æ��VtLp-, (D' 3(a)6 α) (��4dO6��0tS4. (193 A V 211 A)��� 171 A . tLpL�� �� 211 A . � (6 α> 6 β> 6 γ). ���6ttfp�F;�L~z06tf�y6tf4%:0t=[��pXtfA0y6F;otV�(Hg℄Um�t=��

( 3 jn�/ (AR 11092) vNr��qbBxF�b� SDO/AIA C 171 A (a) � 193 A (b) X 211 A (c)psv:s(Fig. 3 A side view on a fan structure image of the active region 11092 obtained by SDO/AIA

in 171 A (a), 193 A (b), and 211 A (c) when crossing the western limb.

4 [�,X $gE��(tfQkm'3%tfM�Z��>r�L� .~w#Cf* -, 34x~*. {Z���O 304 A . tQkp����Z��� 3 min Qk(tfV��I(Qktp�m'Æ �tfA SDO/AIA x~*. 171 A �193 AV 211 A t���d���Jtfh.A1 6�Mt<�T+� .�j~w�1Nm<�T+tp�t�d�>RRtP����Morlet .�j��Æ3��lUAa�,(�e,I4�;�����lUta��?t"K�d�{�?�T�E%lUa�z\t .�j#CtXKlG�{ .�ja�I\0ut MorletQzt��;76 Torrencew [17] tXK�R�1Xortft<�p��>r#'�' 2 h�IwR-,1e�� 2℄�a�t�d'B� .�j��%tft�$���d℄ �>r6��Zg�Yt��4L�$�d+k�:a���,z,�s .�j#C�' 4 7Jtm slit1 �IwR-

32 � 9 � � 54 1,A 171 A . t�� 2℄�a��dt .#C'��h' 4(a) m1e���a�t�d0R�{wR%ht�Y0R��4�$+kat���d0RD' 4(b) �h�' 4(c) 7JX#NOHat���a��dt .<e��{ 99% `EVtNut����';��A 50 min z,#Ct<e�'hGP 3 min tNup�{ 10 �#ktp�lU�NS4p�A6* .<e�h !�P�D' 4(d) �h�\ .<e�' ('4(c)) >ri;��Ptf�� 3 min #tQkp�1mQ{t��m��zJP�I{a��/m 500∼1000 s. \6* .<e� (' 4(d)) tS4&℄;Ytft<�T+!S4p��tnp�m 167 s, �{�Cp� 943 s. 1X���06�Mttf<�p��' 5 V' 6 #'7JX Æ-, 193 A . V 211 A . t .#C'�\'h ;5J�r �℄AS4p� 3 min #ttnp� 1�Nut 10 min #tCp���h� 3 min Qkp� m��JP�I{a��/m 500∼2600 s. ��<e� ('4(c) �' 5(c) V' 6(c)) i;�P� 3 4. t<e� 3zH�q�F�} Æa'1 6�M.tT+!Æ�tUEt�1Xz9tf1 4dO<�p�tÆ t�%1 7JX slit1 � slit2 V slit3 #'A 171 A � 193 A V 211 A 3 4. tQkp��\%h;YtfA 3 4�|4d�{A 3 46�M�℄AS4p�tQk�} 3 min yp�Qk�{ 10 min �OtCp�Qk���I(= 304 A . tQkp�t#CD' 7 �h�' 7(a) 7Jtm4%��I(OÆ4| (' 1(b) _��#4d) tH�0R�\';5J,0R�d*n!tf<��!��t�$+k���1v�0R�Y�L� .�j;\�orZ���AI(=tQkp� 9 3 min. �NOx .#C;Y�tf<�V��I(Qk�℄A3 min Qkp��>r;�); 3 min tfQk;�D3%��Z��Z���t 3 minQk;�RNI(�{N-o`�t [14], ��CttfQkp�;����Qk3w��Y� � 1 .�)�Qb#fD%�8 ("U� s)

Table 1 Comparison of the oscillation periods for different bandpasses (unit: s)

Slit number 171 A 193 A 211 A

Slit1 167/943 166/860 167/604

Slit2 166/882 165/923 196/695

Slit3 166/667 167/930 170/689

5 9>tffOtQkm�z�HtWOR_*T+t�Nm<�T+t)�℄F���m�$��t 4%∼6%. tfht.A Æa'M!z1 tT+���N;�(ft^_=�n t9�^B�ft��VqR1 U�Nh��!E���>r;Jt��1`Æ4�A �z'BM��Na� '>r;� 'JtfT+ttn���>r;JtfA 171 A . t<�T+��� ��T+��A/| 5 arcsec �t��℄�/m 59∼74 km/s; i.��,*T+a����℄&:H �:a�Æ_�℄�{

1 � JP�x�lXX0C\�P!vhjvV- 33

(a) AIA 171 light curve - original

0 1000 2000 3000Time / s

5800

6000

6200

6400

Inte

nsity

(b) AIA 171 light curve - after trend subtraction

0 1000 2000 3000Time / s

-0.02

0.00

0.02

0.04

Rel

.int.

(c) AIA 171 wavelet

0 1000 2000 3000Time / s

100

1000

Per

iod

/ s

99%

99%

(d) global wavelet

0 2x105

Power

100

1000

wavelet analysis

global period at max.

power (<1306 s)

P1=167 s

second highest peak

P2=943 s

( 4 T 1 $�5e (E( 1(a) i) v 171 A 0�ve0%D (a) � (b) (o( 2 jT�}ÆxT[�/.Æ3_vI�1T(�%)o2f{-1TX5M�%,lbv1T( 4(c) o 99% emve0=f�( 4(d) o7+e0%DFig. 4 The wavelet analysis results for slit1 (see Fig.1(a)) in 171 A. Panels (a) and (b) show the light

curves, respectively, the original and background-trend-subtracted, for the region enclosed by horizontal

dashed lines in Fig. 2. Panel (c) shows the wavelet power spectrum with contours enclosing the 99%

confidence regions. Panel (d) is the global wavelet.

34 � 9 � � 54 1(a) AIA 193 light curve - original

0 1000 2000 3000Time / s

3000

3100

3200

3300

3400

3500

Inte

nsity

(b) AIA 193 light curve - after trend subtraction

0 1000 2000 3000Time / s

-0.04

-0.02

0.00

0.02

0.040.06

Rel

.int.

(c) AIA 193 wavelet

0 1000 2000 3000Time / s

100

1000

Per

iod

/ s 99%

99%

(d) global wavelet

0 5x104

Power

100

1000

wavelet analysis

global period at max.

power (<1306 s)

P1=166 s

second highest peak

P2=860 s

( 5 T 1 $�5e (E( 1(a) i) v 193 A 0�ve0%D (a) � (b) (o( 2 jT�}ÆxT[�/.Æ3_vI�1T(�%)o2f{-1TX5M�%,lbv1T( 5(c) o 99% emve0=f�( 5(d) o7+e0%DFig. 5 The wavelet analysis results for slit1 (see Fig.1(a)) in 193 A. Panels (a) and (b) show the light

curves, respectively, the original and background-trend-subtracted, for the region enclosed by horizontal

dashed lines in Fig. 2. Panel (c) shows the wavelet power spectrum with contours enclosing the 99%

confidence regions. Panel (d) is the global wavelet.

1 � JP�x�lXX0C\�P!vhjvV- 35

(a) AIA 211 light curve - original

0 1000 2000 3000Time / s

1300

1350

1400

1450

1500

Inte

nsity

(b) AIA 211 light curve - after trend subtraction

0 1000 2000 3000Time / s

-0.06-0.04-0.020.000.020.040.06

Rel

.int.

(c) AIA 211 wavelet

0 1000 2000 3000Time / s

100

1000

Per

iod

/ s 99%

(d) global wavelet

0 1x104

Power

100

1000

wavelet analysis

global period at max.

power (<1306 s)

P1=167 s

second highest peak

P2=604 s

( 6 T 1 $�5e (E( 1(a) i) v 211 A 0�ve0%D (a) � (b) (o( 2 jT�}ÆxT[�/.Æ3_vI�1T(�%)o2f{-1TX5M�%,lbv1T( 6(c) o 99% emve0=f�( 6(d) o7+e0%DFig. 6 The wavelet analysis results for slit1 (see Fig.1(a)) in 211 A. Panels (a) and (b) show the light

curves, respectively, the original and background-trend-subtracted, for the region enclosed by horizontal

dashed lines in Fig. 2. Panel (c) shows the wavelet power spectrum with contours enclosing the 99%

confidence regions. Panel (d) is the global wavelet.

36 � 9 � � 54 1(a) AIA 304 light curve - original

0 1000 2000 3000Time / s

340360380400420440460

Inte

nsity

(b) AIA 304 light curve - relative intensity

0 1000 2000 3000Time / s

-0.10-0.050.000.050.100.15

Rel

.int.

(c) AIA 304 wavelet

0 1000 2000 3000Time / s

100

1000

Per

iod

/ s 99%

(d) global wavelet

0 5x103

Power

100

1000

wavelet analysis

global period at max.

power(<1306 s)

P=167 s

( 7 \���CK* 304 A 0� (E( 1(b) i) Smve0%D (a) � (b) (o�K`�r “+” $�vSm5vI�1T(�%)o2f{-1TXW���e1T( 7(c) o 99% emve0=f�( 7(d) o7+e0%DFig. 7 The wavelet analysis results for the oscillation period of the umbra (see Fig.1(b)) in 304 A. Panels

(a) and (b) show the light curves of oscillation source denoted by the white cross “+”, the original and

relative intensity, respectively. Panel (c) shows the wavelet power spectrum with contours enclosing the

99% confidence regions. Panel (d) is the global wavelet.

1 � JP�x�lXX0C\�P!vhjvV- 37T+\o/| 20 arcsec O���℄�/m 80∼121 km/s. ( 171 A . 1 tm�tfh4% 193 A V 211 A S4. tT+��A/| 2 arcsec O� ��z5��1<�t��T+�.tT+/G�����℄t�/#'m 46∼59 km/s V 40∼58 km/s.�N��0y6��MtftT+���T�06. F;ot<�:C�|��Nm<�T+mÆmj.��1m�g`�>rortfF;��2 %V��6b$�f��NURmj.}n�/�t�tf<�T+��A06. tF;���y6. �Nm�106tf 193 A V 211 A t(S4%:0t=[�Nhft$�: �D$���:y�Y*�>ri�P 171 A . �{ 193 A . a� 'h�!��qM���T�Nhva%ztfhtjWV.1�m�_����tf_*T+��:1 6�tft<�T+��!?��hm�r℄Ar�U t<�p��}� 3 min1tt�p�Qk{ 10 min #tCp�Qk�1�tf℄A 3 min p�tt<��I(=tZ���- ℄AF�p�tQk��Y�>r);NmtfQk3%Z����Z���t 3 min Qkm;��NI(�{N-o`y�tt�_*�!Etfh℄AtCp�Qk℄;�J���tQk3�Niv�:�tF;{Zt�(�{~w��t.�� � ; V Y[1] Ofman L, Romoli M, Poletto G, et al. ApJ, 1997, 491: L111

[2] DeForest C E, Gurman J B. ApJ, 1998, 501: L217

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[6] Krishna Prasad S, Banerjee D, Gupta G R. A&A, 2011, 528: L4

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38 � 9 � � 54 1Propagation of the Slow Magnetoacoustic Waves in

Coronal Loops above the Sunspot

LI Hai-dong1 ZHAO Li1 LIANG Hong-fei1 BI Yi2 HONG Jun-chao2

ZHENG Rui-sheng2

(1 School of Physics & Electronic Information Technology, Yunnan Normal University, Kunming 650500)

(2 Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming 650011)

ABSTRACT The observations from the Atmospheric Imaging Assembly (AIA) onboard the

Solar Dynamics Observatory (SDO) reveal the weak propagating disturbances (PDs) in the

fan-like coronal loops of the active region (AR 11092) in 171 A, 193 A, and 211 A. These

PDs seem to be a common phenomenon in this part of the active region. The disturbances

originate from small-scale brightenings at the footpoints of the loops and propagate along

the loops. The observed propagation speeds decreased when the PDs were propagating in

hotter plasmas. It roughly varies between 40 km/s and 121 km/s for three bandpasses, which

is close to and below the expected sound speed in the coronal loops. Considering the pro-

jection effect and different angles to our line of sight, it is exactly what the slow-wave model

expects. The wavelet analysis does not show a significant difference among the periods of

the PDs observed in different bandpasses. The periodic patterns of two distinct periods, 3

min and more than 10 min, are detected in three bandpasses. Not only the coronal loops

but also the sunspot regions on the chromosphere display intensity oscillations with a period

of the order of 3 min. This result suggests that the sunspot oscillations can propagate into

the corona through the chromospheres and the transition region.

Key words sun: corona, sun: oscillations, sun: UV radiation, sun: transition region,

waves