Sunspots appear dark because they are hotter than the sur- rounding gas of the photosphere. (T/F)
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- A Crude Analysis: In about 5 billion years, the Sun is going to look a lot different. Our sun is going to turn into a red-giant, a bigger star whose core temperature is much higher than the Sun's current core temperature (you will learn about the red giants in the coming weeks). Assume the core temperature of the red-giant phase of the Sun does not go beyond 100 million degrees. Do you think the temperature is high enough for helium fusion to occur? Note that this question is about helium fusion not hydrogen fusion. How are you going about proving your claim? Question: What temperature in degrees Kelvin must the red-giant sun be at to allow for the helium-helium interactions to take place not considering the Quantum Mechanical effects (i.e. what temperature would allow helium atoms to breach the helium-helium potential wall without help from Quantum Mechanics)? Use wolfram alpha to find the values for the constants. Round your answer to two decimal places. Your answer i [ Select ] 1.47…The Sun will get brighter as it begins to run out of fuel in its core. (T/F)Flares are caused by magnetic disturbances in the lower atmo- sphere of the Sun. (T/F)
- If the temperature at the centre of the sun is 15,000,000 K and the temperature of the photosphere is 5,800 K, what is the ratio of the temperature at the centre of the Sun compared to the photosphere? Express your final answer in the fully factorised form x : 1, where x is a number that you should determine to an appropriate number of significant figures and write it using scientific notation.1) What is thermal equilibrium? Is the Sun in thermal equilibrium? How do we know this? 2) In order to maintain thermal equilibrium, how much energy must the Sun generate every second?Assume that the solar wind causes the Sun to lose mass at a rate of 2 x 10’ kg/s. If you assume the wind is emitted a constant rate, estimate the time (in units of Gyr =Gigayears = 10° years) that it will take the entire Sun to evaporate via its solar wind emission. (Of course, the rate won't be constant throughout the lifetime of the Sun---this is just a rough estimate to understand the timescale associated with this process.) [Hint: you need to look up a number and do several unit conversions; this is a *rate* problem. Enter your answer as an integer or decimal, NOT in scientific notation.]