Observational and numerical characterization of a recurrent arc-shaped front propagating along a coronal fan
Context. Recurrent, arc-shaped intensity disturbances were detected by extreme-ultraviolet channels in an active region. The fronts were observed to propagate along a coronal loop bundle rooted in a small area within a sunspot umbra. Previous works have linked these intensity disturbances to slow ma...
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Published in | Astronomy and astrophysics (Berlin) Vol. 667; p. A21 |
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Main Authors | , , , , , , , |
Format | Journal Article |
Language | English |
Published |
Heidelberg
EDP Sciences
01.11.2022
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Abstract | Context.
Recurrent, arc-shaped intensity disturbances were detected by extreme-ultraviolet channels in an active region. The fronts were observed to propagate along a coronal loop bundle rooted in a small area within a sunspot umbra. Previous works have linked these intensity disturbances to slow magnetoacoustic waves that propagate from the lower atmosphere to the corona along the magnetic field.
Aims.
The slow magnetoacoustic waves propagate at the local cusp speed, which is equivalent to the sound speed in a low-
β
-regime plasma. However, the measured propagation speeds from the intensity images are usually smaller as they are subject to projection effects due to the inclination of the magnetic field with respect to the line of sight. We aim to understand the effect of projection by comparing observed speeds with those from a numerical model.
Methods.
Using multi-wavelength data, we determined the periods present in the observations at different heights of the solar atmosphere through Fourier analysis. We calculated the plane-of-sky speeds along one of the loops from the cross-correlation time-lags obtained as a function of distance along the loop. We performed a 2D ideal magnetohydrodynamic simulation of an active region embedded in a stratified atmosphere. We drove slow waves from the photosphere with a three-minute periodicity. Synthetic time–distance maps were generated from the forward-modelled intensities in coronal wavelengths and the projected propagation speeds were calculated.
Results.
The intensity disturbances show a dominant period between 2 and 3 min at different heights of the atmosphere. The apparent propagation speeds calculated for coronal channels exhibit an accelerated pattern with values increasing from 40 to 120 km s
−1
as the distance along the loop rises. The propagation speeds obtained from the synthetic time–distance maps also exhibit accelerated profiles within a similar range of speeds.
Conclusions.
We conclude that the accelerated propagation in our observations is due to the projection effect. |
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AbstractList | Context. Recurrent, arc-shaped intensity disturbances were detected by extreme-ultraviolet channels in an active region. The fronts were observed to propagate along a coronal loop bundle rooted in a small area within a sunspot umbra. Previous works have linked these intensity disturbances to slow magnetoacoustic waves that propagate from the lower atmosphere to the corona along the magnetic field. Aims. The slow magnetoacoustic waves propagate at the local cusp speed, which is equivalent to the sound speed in a low-β-regime plasma. However, the measured propagation speeds from the intensity images are usually smaller as they are subject to projection effects due to the inclination of the magnetic field with respect to the line of sight. We aim to understand the effect of projection by comparing observed speeds with those from a numerical model. Methods. Using multi-wavelength data, we determined the periods present in the observations at different heights of the solar atmosphere through Fourier analysis. We calculated the plane-of-sky speeds along one of the loops from the cross-correlation time-lags obtained as a function of distance along the loop. We performed a 2D ideal magnetohydrodynamic simulation of an active region embedded in a stratified atmosphere. We drove slow waves from the photosphere with a three-minute periodicity. Synthetic time–distance maps were generated from the forward-modelled intensities in coronal wavelengths and the projected propagation speeds were calculated. Results. The intensity disturbances show a dominant period between 2 and 3 min at different heights of the atmosphere. The apparent propagation speeds calculated for coronal channels exhibit an accelerated pattern with values increasing from 40 to 120 km s−1 as the distance along the loop rises. The propagation speeds obtained from the synthetic time–distance maps also exhibit accelerated profiles within a similar range of speeds. Conclusions. We conclude that the accelerated propagation in our observations is due to the projection effect. Context. Recurrent, arc-shaped intensity disturbances were detected by extreme-ultraviolet channels in an active region. The fronts were observed to propagate along a coronal loop bundle rooted in a small area within a sunspot umbra. Previous works have linked these intensity disturbances to slow magnetoacoustic waves that propagate from the lower atmosphere to the corona along the magnetic field. Aims. The slow magnetoacoustic waves propagate at the local cusp speed, which is equivalent to the sound speed in a low- β -regime plasma. However, the measured propagation speeds from the intensity images are usually smaller as they are subject to projection effects due to the inclination of the magnetic field with respect to the line of sight. We aim to understand the effect of projection by comparing observed speeds with those from a numerical model. Methods. Using multi-wavelength data, we determined the periods present in the observations at different heights of the solar atmosphere through Fourier analysis. We calculated the plane-of-sky speeds along one of the loops from the cross-correlation time-lags obtained as a function of distance along the loop. We performed a 2D ideal magnetohydrodynamic simulation of an active region embedded in a stratified atmosphere. We drove slow waves from the photosphere with a three-minute periodicity. Synthetic time–distance maps were generated from the forward-modelled intensities in coronal wavelengths and the projected propagation speeds were calculated. Results. The intensity disturbances show a dominant period between 2 and 3 min at different heights of the atmosphere. The apparent propagation speeds calculated for coronal channels exhibit an accelerated pattern with values increasing from 40 to 120 km s −1 as the distance along the loop rises. The propagation speeds obtained from the synthetic time–distance maps also exhibit accelerated profiles within a similar range of speeds. Conclusions. We conclude that the accelerated propagation in our observations is due to the projection effect. |
Author | Costa, A. Van Doorsselaere, T. Krishna Prasad, S. Stenborg, G. Esquivel, A. Sieyra, M. V. Riedl, J. M. Khomenko, E. |
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References | Reznikova (R44) 2012; 746 Marsh (R32) 2006; 643 Yuan (R57) 2012; 543 Sheeley (R48) 2014; 797 DeForest (R14) 1998; 501 Vögler (R54) 2005; 429 Jess (R24) 2013; 779 Reznikova (R43) 2012; 756 Jess (R23) 2012; 746 Misra (R35) 2018; 23 González-Morales (R19) 2019; 870 Hu (R21) 2001; 173 Ofman (R38) 1997; 476 R1 Kobanov (R27) 2013; 554 Banerjee (R2) 2021; 217 Fedun (R15) 2011; 727 De Moortel (R12) 2015; 290 Fleck (R17) 1991; 250 Wang (R56) 2009; 503 Berghmans (R5) 1999; 186 Zurbriggen (R61) 2020; 494 Van Doorsselaere (R52) 2016; 3 Felipe (R16) 2010; 719 Botha (R7) 2011; 728 Krishna Prasad (R29) 2015; 812 Mumford (R36) 2015; 799 De Moortel (R10) 2012; 370 De Moortel (R11) 2002; 387 Berenger (R4) 1996; 127 Wang (R55) 2016; 216 Santamaria (R46) 2015; 577 Zhukov (R60) 2002; 386 De Pontieu (R13) 2010; 722 Khomenko (R26) 2018; 618 Marsh (R33) 2009; 706 Schou (R47) 2012; 275 Bogdan (R6) 2000; 192 R42 Sych (R50) 2009; 505 R49 Tomczyk (R51) 2009; 697 Yuan (R58) 2014; 561 Nakariakov (R37) 2020; 58 González-Morales (R18) 2018; 615 Jess (R22) 2012; 757 Chae (R8) 2017; 836 Krishna Prasad (R28) 2012; 281 Cho (R9) 2019; 879 Lemen (R31) 2012; 275 Khomenko (R25) 2009; 694 Riedl (R45) 2021; 922 Van Doorsselaere (R53) 2020; 216 Parchevsky (R39) 2007; 666 Zhao (R59) 2016; 830 Pesnell (R41) 2012; 275 Marsh (R34) 2009; 697 Parchevsky (R40) 2009; 694 Hu (R20) 1996; 129 Krishna Prasad (R30) 2017; 834 Berenger (R3) 1994; 114 |
References_xml | – volume: 799 start-page: 6 year: 2015 ident: R36 publication-title: ApJ doi: 10.1088/0004-637X/799/1/6 contributor: fullname: Mumford – volume: 216 start-page: 140 year: 2020 ident: R53 publication-title: Space Sci. Rev. doi: 10.1007/s11214-020-00770-y contributor: fullname: Van Doorsselaere – volume: 275 start-page: 17 year: 2012 ident: R31 publication-title: Sol. Phys. doi: 10.1007/s11207-011-9776-8 contributor: fullname: Lemen – volume: 505 start-page: 791 year: 2009 ident: R50 publication-title: A&A doi: 10.1051/0004-6361/200912132 contributor: fullname: Sych – volume: 697 start-page: 1674 year: 2009 ident: R34 publication-title: ApJ doi: 10.1088/0004-637X/697/2/1674 contributor: fullname: Marsh – volume: 719 start-page: 357 year: 2010 ident: R16 publication-title: ApJ doi: 10.1088/0004-637X/719/1/357 contributor: fullname: Felipe – volume: 186 start-page: 207 year: 1999 ident: R5 publication-title: Sol. Phys. doi: 10.1023/A:1005189508371 contributor: fullname: Berghmans – volume: 23 start-page: 83 year: 2018 ident: R35 publication-title: Astron. Comput. doi: 10.1016/j.ascom.2018.03.002 contributor: fullname: Misra – volume: 615 start-page: A67 year: 2018 ident: R18 publication-title: A&A doi: 10.1051/0004-6361/201731916 contributor: fullname: González-Morales – volume: 812 start-page: L15 year: 2015 ident: R29 publication-title: ApJ doi: 10.1088/2041-8205/812/1/L15 contributor: fullname: Krishna Prasad – volume: 577 start-page: A70 year: 2015 ident: R46 publication-title: A&A doi: 10.1051/0004-6361/201424701 contributor: fullname: Santamaria – volume: 275 start-page: 229 year: 2012 ident: R47 publication-title: Sol. Phys. doi: 10.1007/s11207-011-9842-2 contributor: fullname: Schou – ident: R42 – volume: 114 start-page: 185 year: 1994 ident: R3 publication-title: J. Comput. Phys. doi: 10.1006/jcph.1994.1159 contributor: fullname: Berenger – volume: 834 start-page: 103 year: 2017 ident: R30 publication-title: ApJ doi: 10.3847/1538-4357/834/2/103 contributor: fullname: Krishna Prasad – volume: 746 start-page: 119 year: 2012 ident: R44 publication-title: ApJ doi: 10.1088/0004-637X/746/2/119 contributor: fullname: Reznikova – ident: R49 – volume: 779 start-page: 168 year: 2013 ident: R24 publication-title: ApJ doi: 10.1088/0004-637X/779/2/168 contributor: fullname: Jess – volume: 429 start-page: 335 year: 2005 ident: R54 publication-title: A&A doi: 10.1051/0004-6361:20041507 contributor: fullname: Vögler – volume: 543 start-page: A9 year: 2012 ident: R57 publication-title: A&A doi: 10.1051/0004-6361/201218848 contributor: fullname: Yuan – ident: R1 – volume: 836 start-page: 18 year: 2017 ident: R8 publication-title: ApJ doi: 10.3847/1538-4357/836/1/18 contributor: fullname: Chae – volume: 757 start-page: 160 year: 2012 ident: R22 publication-title: ApJ doi: 10.1088/0004-637X/757/2/160 contributor: fullname: Jess – volume: 756 start-page: 35 year: 2012 ident: R43 publication-title: ApJ doi: 10.1088/0004-637X/756/1/35 contributor: fullname: Reznikova – volume: 217 start-page: 76 year: 2021 ident: R2 publication-title: Space Sci. Rev. doi: 10.1007/s11214-021-00849-0 contributor: fullname: Banerjee – volume: 706 start-page: L76 year: 2009 ident: R33 publication-title: ApJ doi: 10.1088/0004-637X/706/1/L76 contributor: fullname: Marsh – volume: 58 start-page: 441 year: 2020 ident: R37 publication-title: ARA&A doi: 10.1146/annurev-astro-032320-042940 contributor: fullname: Nakariakov – volume: 370 start-page: 3193 year: 2012 ident: R10 publication-title: Phil. Trans. Roy. Soc. London Ser. A contributor: fullname: De Moortel – volume: 3 start-page: 4 year: 2016 ident: R52 publication-title: Front. Astron. Space Sci. doi: 10.3389/fspas.2016.00004 contributor: fullname: Van Doorsselaere – volume: 797 start-page: 131 year: 2014 ident: R48 publication-title: ApJ doi: 10.1088/0004-637X/797/2/131 contributor: fullname: Sheeley – volume: 694 start-page: 573 year: 2009 ident: R40 publication-title: ApJ doi: 10.1088/0004-637X/694/1/573 contributor: fullname: Parchevsky – volume: 290 start-page: 399 year: 2015 ident: R12 publication-title: Sol. Phys. doi: 10.1007/s11207-014-0610-y contributor: fullname: De Moortel – volume: 127 start-page: 363 year: 1996 ident: R4 publication-title: J. Comput. Phys. doi: 10.1006/jcph.1996.0181 contributor: fullname: Berenger – volume: 830 start-page: L17 year: 2016 ident: R59 publication-title: ApJ doi: 10.3847/2041-8205/830/1/L17 contributor: fullname: Zhao – volume: 722 start-page: 1013 year: 2010 ident: R13 publication-title: ApJ doi: 10.1088/0004-637X/722/2/1013 contributor: fullname: De Pontieu – volume: 561 start-page: A19 year: 2014 ident: R58 publication-title: A&A doi: 10.1051/0004-6361/201220208 contributor: fullname: Yuan – volume: 216 start-page: 395 year: 2016 ident: R55 publication-title: Geophys. Union Geophys. Monograph Ser. doi: 10.1002/9781119055006.ch23 contributor: fullname: Wang – volume: 387 start-page: L13 year: 2002 ident: R11 publication-title: A&A doi: 10.1051/0004-6361:20020436 contributor: fullname: De Moortel – volume: 192 start-page: 373 year: 2000 ident: R6 publication-title: Sol. Phys. doi: 10.1023/A:1005225214520 contributor: fullname: Bogdan – volume: 666 start-page: 547 year: 2007 ident: R39 publication-title: ApJ doi: 10.1086/520108 contributor: fullname: Parchevsky – volume: 643 start-page: 540 year: 2006 ident: R32 publication-title: ApJ doi: 10.1086/501450 contributor: fullname: Marsh – volume: 129 start-page: 201 year: 1996 ident: R20 publication-title: J. Comput. Phys. doi: 10.1006/jcph.1996.0244 contributor: fullname: Hu – volume: 746 start-page: 183 year: 2012 ident: R23 publication-title: ApJ doi: 10.1088/0004-637X/746/2/183 contributor: fullname: Jess – volume: 503 start-page: L25 year: 2009 ident: R56 publication-title: A&A doi: 10.1051/0004-6361/200912534 contributor: fullname: Wang – volume: 275 start-page: 3 year: 2012 ident: R41 publication-title: Sol. Phys. doi: 10.1007/s11207-011-9841-3 contributor: fullname: Pesnell – volume: 281 start-page: 67 year: 2012 ident: R28 publication-title: Sol. Phys. contributor: fullname: Krishna Prasad – volume: 697 start-page: 1384 year: 2009 ident: R51 publication-title: ApJ doi: 10.1088/0004-637X/697/2/1384 contributor: fullname: Tomczyk – volume: 173 start-page: 455 year: 2001 ident: R21 publication-title: J. Comput. Phys. doi: 10.1006/jcph.2001.6887 contributor: fullname: Hu – volume: 554 start-page: A146 year: 2013 ident: R27 publication-title: A&A doi: 10.1051/0004-6361/201220548 contributor: fullname: Kobanov – volume: 618 start-page: A87 year: 2018 ident: R26 publication-title: A&A doi: 10.1051/0004-6361/201833048 contributor: fullname: Khomenko – volume: 727 start-page: 17 year: 2011 ident: R15 publication-title: ApJ doi: 10.1088/0004-637X/727/1/17 contributor: fullname: Fedun – volume: 494 start-page: 5270 year: 2020 ident: R61 publication-title: MNRAS doi: 10.1093/mnras/staa1105 contributor: fullname: Zurbriggen – volume: 728 start-page: 84 year: 2011 ident: R7 publication-title: ApJ doi: 10.1088/0004-637X/728/2/84 contributor: fullname: Botha – volume: 870 start-page: 94 year: 2019 ident: R19 publication-title: ApJ doi: 10.3847/1538-4357/aaf1a9 contributor: fullname: González-Morales – volume: 476 start-page: L51 year: 1997 ident: R38 publication-title: ApJ doi: 10.1086/310491 contributor: fullname: Ofman – volume: 386 start-page: 653 year: 2002 ident: R60 publication-title: A&A doi: 10.1051/0004-6361:20020279 contributor: fullname: Zhukov – volume: 879 start-page: 67 year: 2019 ident: R9 publication-title: ApJ doi: 10.3847/1538-4357/ab2466 contributor: fullname: Cho – volume: 694 start-page: 411 year: 2009 ident: R25 publication-title: ApJ doi: 10.1088/0004-637X/694/1/411 contributor: fullname: Khomenko – volume: 250 start-page: 235 year: 1991 ident: R17 publication-title: A&A contributor: fullname: Fleck – volume: 922 start-page: 225 year: 2021 ident: R45 publication-title: ApJ doi: 10.3847/1538-4357/ac23c7 contributor: fullname: Riedl – volume: 501 start-page: L217 year: 1998 ident: R14 publication-title: ApJ doi: 10.1086/311460 contributor: fullname: DeForest |
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Recurrent, arc-shaped intensity disturbances were detected by extreme-ultraviolet channels in an active region. The fronts were observed to propagate... Context. Recurrent, arc-shaped intensity disturbances were detected by extreme-ultraviolet channels in an active region. The fronts were observed to propagate... |
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SubjectTerms | Channels Coronal loops Cross correlation Disturbances Fluid flow Fourier analysis Lower atmosphere Magnetic fields Magnetoacoustic waves Magnetohydrodynamic simulation Mathematical models Numerical methods Numerical models Photosphere Propagation Solar atmosphere Sound propagation Sunspots Wave propagation |
Title | Observational and numerical characterization of a recurrent arc-shaped front propagating along a coronal fan |
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