Izvleček
Sonce, naša najbližja zvezda, je v obdobjih povečane magnetne aktivnosti posuto s številnimi pegami, ki nastanejo zaradi motenj v Sončevem magnetnem polju. Pege se premikajo preko Sončeve ploskvice skupaj s Sončevo snovjo, ker se Sonce vrti okoli lastne osi. S šolsko opremo: 20-centimetrskim Newtonovim teleskopom, zaščitnim steklenim filtrom Thousand Oaks in digitalnim fotoaparatom Canon EOS 700D s snemljivim objektivom, smo več dni zapored fotografirali aktivno Sonce in spremljali premike izbranih peg. Te posnetke smo obdelali in analizirali, pri čemer smo intenziteto svetlobe povezali s funkcijo izvira in s Planckovo funkcijo, da smo ocenili temperaturo v osrednjih predelih izbranih Sončevih peg. V prvem delu članka so predstavljene osnovne informacije o Soncu, Sončevih pegah in opravljenih meritvah, medtem ko se bo drugi del članka osredotočil na obdelavo posnetkov in določitev temperature v osrednjih predelih Sončevih peg.
Abstract
Estimation of Sunspot Temperatures With Simple School Equipment (Part 1)
The Sun is the closest star to Earth. During periods of heightened magnetic activity, multiple sunspots form due to disturbances in the Sun’s magnetic field. These sunspots move across the Sun’s surface along with its material as the Sun rotates on its axis. We captured images of the Sun using basic school equipment, including a 20 cm Newtonian telescope, a Thousand Oaks glass filter, and a Canon EOS 700D digital camera. These images can be processed and analysed. We estimated sunspot temperatures by relating light intensity to the source function and Planck’s function. This article contains two parts. Part 1 introduces the Sun, sunspots, and the measurements we conducted, while Part 2 covers digital image processing and temperature determination in sunspots.