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بررسی مکانیزم گرمایشی لوله‌های داغ تاج به‌کمک مطالعه طیفی و تصویری نواحی موس خورشیدی | ||
| فیزیک زمین و فضا | ||
| مقاله 13، دوره 49، شماره 3، آبان 1402، صفحه 747-764 اصل مقاله (2.54 M) | ||
| نوع مقاله: مقاله پژوهشی | ||
| شناسه دیجیتال (DOI): 10.22059/jesphys.2023.351790.1007488 | ||
| نویسندگان | ||
| شادی محسنی؛ ندا داداشی* | ||
| گروه فیزیک، دانشکده علوم، دانشگاه زنجان، زنجان، ایران. | ||
| چکیده | ||
| نواحی فعال تاج که لنگرگاه‌های مغناطیسی خورشید هستند به دو زیر بخش کلی تقسیم می‌شوند: لوله‌های گرم با دمای 1 مگا کلوین و لوله‌های داغ با دمای بیش از 5/1 مگا کلوین. شواهد رصدی بسیاری وجود دارد که گرمایش در لوله‌های گرم از طریق مدل یکنواخت نانوشراره‌ای ایجاد می‌شود اما پهنای ذاتی خطوط نشری گسیل‌شده از تاج، امکان تعیین دقیق نوع گرمایش را در لوله‌های داغ در هاله‌ای از ابهام نهاده است. از این‌رو برای مطالعه مکانیزم گرمایشی لوله‌های داغ بر نواحی پایه این لوله‌ها که نواحی موس (Moss) نامیده می‌شود، تمرکز می‌کنند. به‌کمک داده‌های تلسکوپ فضایی آیریس و اِس دی او به بررسی تحول دینامیکی و طیفی نواحی موس از یک ناحیه فعال پرداخته‌ایم. نتایج تحلیل نوسانات به روش فوریه روی نواحی موس، نوساناتی با دوره‌تناوب‌های مشترک 9/3 و 9/6 دقیقهای را در پهنا، شدت و سرعت دوپلری خطوط طیفی C II و Si IV نشان می‌دهد. نوسانات 9/3 دقیقهای در کانال داغAIA 211 نیز دیده شدند که می‌تواند مربوط به حضور امواج آلفن پیچشی کوپل شده با امواج مغناطودینامیکی کینک باشد که نهایتاً می‌تواند منجر به گرمایش تاجی از نوع موجی در ساختارهای موس شود. دوره‌تناوب‌های کوتاه بین 9/0 تا 2 دقیقهای نیز در کانال‌های با دمای بالاتر AIA 335 و 131 و 94 و برخی کانال‌های با دمای میانی مشاهده شد که می‌تواند مربوط به بازاتصالی‌های مغناطیسی متوالی در لایه‌های بالای تاجی باشد. این بازاتصالی‌ها می‌توانند به‌عنوان عاملی برای تحریک و انتشار امواج آلفن مشاهده شده باشند. | ||
| کلیدواژه‌ها | ||
| پلاسما؛ ناحیه فعال؛ امواج مغناطوهیدرودینامیک؛ نوسانات | ||
| عنوان مقاله [English] | ||
| Investigating the Heating Mechanism of Hot Coronal Loops Using Spectral and Imaging Analysis of the Solar Moss Areas | ||
| نویسندگان [English] | ||
| Shadi Mohseni؛ Neda Dadashi | ||
| Department of Physics, Faculty of Science, University of Zanjan, Zanjan, Iran. | ||
| چکیده [English] | ||
| Coronal heating mechanisms are generally classified as waves (AC: Alternating Current) and Direct Current (DC) models. Restricted evidences from both models have been observed over different structures of the solar atmosphere. However, a general model describing the global heating process in the whole solar atmosphere is missing. Active regions are the magnetic anchorages of the solar corona. It is believed that the Active Regions have important contribution in the heating of the corona. ARs are divided into two sub-regions: Warm coronal loops (~ 1 MK) and hot coronal loops (> 1.5 MK). There are strong observational evidence supporting the DC nanoflare model in the warm coronal loops. However, there is still no conclusive answer for the responsible heating mechanism of hot loops. There are some observational evidence indicating the existence of steady heating, some others indicating the impulsive heating, and very lately people have found MHD wave heating signatures in the hot loops. The intrinsic fuzzy nature of hot coronal emission lines made it impossible to isolate the hot loop structures and study their physical properties separately. Therefore, the only way to study the hot loops is to focus on their hot footpoints called “moss” areas, which was discovered in 1999 by Berger et al. using TRACE 171 Å images. The moss emission has a reticulated spongy structure. It is believed that when the hot coronal loops cover the cold plage regions, an inward radial thermal conduction gradient is formed which causes the plasma to heat up and radiate. This radiation is what we call ”moss”. The dark patches inside the bright moss areas are the cross sections of the cold spicular materials rising upward toward the corona. Using spectroscopic and imaging data of Interface Region Imaging Spectrograph (IRIS) and Solar Dynamic Observatory (SDO), dynamic properties of the moss areas over an AR is studied. Three boxes of moss regions are selected. The time variation of the intensity, Doppler shift, and line widths of C II 1335.7077 Å and Si IV 1402.770 Å emission lines are investigated. Time series of the intensities over the three selected moss regions are made from IRIS SJI 1400, and 2796, along with AIA/SDO 1700, 304, 1600, 171, 193, 211, 335, 94, and 131 channels. Using FFT technique we obtained oscillatory behavior over the all mentioned parameters. The results show oscillatory behaviors in the line width, Doppler shifts, and line intensities of C II and Si IV spectral lines with periods of 3.9 and 6.9 minutes over the moss areas. 3.9 min oscillations are observed over the AIA 211 passband, as well, which could be an indication of the presence of torsional Alfven waves coupled with kind mode. High frequency oscillations with 0.9 to 2 min periods are observed over the selected moss regions in AIA hot channels like 335, 131, and 94, as well as Si IV line. This could be an indication of occurring magnetic reconnections above the moss regions in the hot coronal lines, triggering the Alfven waves in this structure. Therefore, our results support the presence of MHD waves heating mechanisms in the studied moss structures. | ||
| کلیدواژه‌ها [English] | ||
| Plasma, Active Region, MHD waves, Oscillations | ||
| مراجع | ||
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