رفتار تناوبی درخشندگی‌های سریع در مقیاس کوچک بر روی دیسک خورشید

در این تحقیق، رفتار تناوبی درخشندگی‌های سریع در مقیاس کوچک را با استفاده از تصاویر دیسک خورشید که توسط تلسکوپ فضایی آیریس استخراج شده، در طول موج های 1400و1330 ،2796 آنگستروم بررسی می‌کنیم. مطالعه این نقاط درخشان ما را به هویت واقعی آنها و تاثیر این نقاط بر روی رویدادهای گذرا در جو خورشید آگاه می سازد. نقاط روشن شبکه که توسط صافی‌های خاص قابل مشاهده هستند در طرح‌های تقریباً سلولی که مرزهای شبکه را می‌سازند مرتب شده‌اند. این نقاط درخشان چشمه هایی با عمر کوتاه پلاسمایی هستند که از رنگین‌سپهر یا جو پایین‌تر خورشید منشا می‌گیرند .با تحلیل نوسانات شدت این نقاط به‌روش موجک به دوره تناوب آنها می‌توان پی برد. با توجه به نتایج تحلیل موجک پیک‌ها‌ی سه و پنج دقیقه‌ای شناسایی شد. پیک‌های سه دقیقه‌ای رنگین‌سپهر و پنج دقیقه‌ای شیدسپهر که در این تحقیق آشکار شد، نشان می‌دهد که نوسانات شدت نقاط روشن از نوع مدهای p هستند که منشا آنها مدهای فشاری است. در نوسانات سه دقیقه‌ای منشا رنگین‌سپهر و در پنج دقیقه‌ای منشا شید سپهر دارند. همچنین برای بدست آوردن سرعت‌های دوپلری از تصاویر طیفی استفاده شد و این سرعت‌ها در محدوده 20- الی 30 کیلومتر بر ثانیه محاسبه شده است. نتایج این مطالعه نشان داد که این نقاط درخشان چشمه‌های نوسانی کوتاه مدت پلاسمایی هستند که از کروموسفر یا جو پایینی خورشید منشا می‌گیرند.

periodic behavior of fast small-scale brightening on the solar disk

a distinct difference is seen between different parts of the solar  chromosphere, including the bright points (bps) at the boundary and within the network, and the darker regions formed the interior of the granules. in the photosphere, apart from sunspots and holes, there are direct and concentrated magnetic fields in the form of small flux tubes with fields of 1 to 2 kg. chromospheric networks are highly dynamic regions with fine structures embedded in the magnetic flux. these structures are located inside the cell network and there are also many small and dark cells around it. bps can be thought of as trails of spicules through which mass and energy from the lower layers of the sun are transported to the corona as the solar wind. although in the last two decades, despite high-resolution observations and theoretical advances, effective steps have been taken to determine dynamics of bps and various thermodynamic parameters such as temperature and density, but the mechanisms responsible for their formation are still unknown. these ambiguities are due to the difference in their appearance as a result of observation at different spectral lines and wavelengths. in terms of their dimensions, lifetimes and physical conditions, there is indirect evidence that there is a relationship between the identity of spicules and bps of the chromospheric network, which can be attributed to the position of the magnetic field around the points. bps form smaller or larger groups that, due to their specific morphology, carry plasma flux tubes to the magnetic corona. the flow behavior along bps and spikes is a debatable issue. however, observations of the contents of the sticks show periodic up and down movements. in this research, using images of the solar disc extracted by the iris space telescope, we investigate the periodic behavior of fast brightening on a small scale. by analyzing the movements of these points using the wavelet method, one can understand their periodicity. examining these points in wavelengths of 1400, 1330, 2796 å to the real identity and the effect of these points on the reactions obtained by the sun. the bright points of the grid are arranged for the light grains visible in the filters and in the roughly cellular designs that form the boundaries of the grid. according to the graphs of wavelet analysis, the three-minute peaks are quite clear. the 3-minute and 5-minute chromospheric peaks seen in these analyzes show that the considered bright points are p modes, which means compression mode. in the three-minute oscillations, the origin is chromospheric, and in the five-minute oscillations, the origin is photosphere. origin of the p modes is (5-minute fluctuations) compressive forces. spectral images were used to obtain doppler velocities and these velocities were calculated as -20  to 30 km-1. the results of this study suggested that these bright points are short-lived sources of plasma that originate from the chromosphere or the lower atmosphere of the sun.