EBK UNDERSTANDING OUR UNIVERSE (THIRD E
3rd Edition
ISBN: 9780393631760
Author: Blumenthal
Publisher: VST
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Chapter 11, Problem 33QAP
To determine
The problem of solar neutrino and the method through which it was solved.
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Explain why there is the low number of observed solar neutrinos?
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.]
Considering your answer to the above question, how does this timescale for the Sun's evaporation by the solar wind compare to the age of the
Universe?
O The solar wind evaporation time is much longer than the age of the Universe
O The solar wind evaporation time is much shorter than the age of the Universe.
O The solar wind evaporation time is close to the age of the Universe (ie, within a few billion years
Chapter 11 Solutions
EBK UNDERSTANDING OUR UNIVERSE (THIRD E
Ch. 11.1 - Prob. 11.1CYUCh. 11.2 - Prob. 11.2CYUCh. 11.3 - Prob. 11.3CYUCh. 11.4 - Prob. 11.4CYUCh. 11 - Prob. 1QAPCh. 11 - Prob. 2QAPCh. 11 - Prob. 3QAPCh. 11 - Prob. 4QAPCh. 11 - Prob. 5QAPCh. 11 - Prob. 6QAP
Ch. 11 - Prob. 7QAPCh. 11 - Prob. 8QAPCh. 11 - Prob. 9QAPCh. 11 - Prob. 10QAPCh. 11 - Prob. 11QAPCh. 11 - Prob. 12QAPCh. 11 - Prob. 13QAPCh. 11 - Prob. 14QAPCh. 11 - Prob. 15QAPCh. 11 - Prob. 16QAPCh. 11 - Prob. 17QAPCh. 11 - Prob. 18QAPCh. 11 - Prob. 19QAPCh. 11 - Prob. 20QAPCh. 11 - Prob. 21QAPCh. 11 - Prob. 22QAPCh. 11 - Prob. 23QAPCh. 11 - Prob. 24QAPCh. 11 - Prob. 25QAPCh. 11 - Prob. 26QAPCh. 11 - Prob. 27QAPCh. 11 - Prob. 28QAPCh. 11 - Prob. 29QAPCh. 11 - Prob. 30QAPCh. 11 - Prob. 31QAPCh. 11 - Prob. 32QAPCh. 11 - Prob. 33QAPCh. 11 - Prob. 34QAPCh. 11 - Prob. 35QAPCh. 11 - Prob. 36QAPCh. 11 - Prob. 37QAPCh. 11 - Prob. 38QAPCh. 11 - Prob. 39QAPCh. 11 - Prob. 40QAPCh. 11 - Prob. 41QAPCh. 11 - Prob. 42QAPCh. 11 - Prob. 43QAPCh. 11 - Prob. 44QAPCh. 11 - Prob. 45QAP
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- Someone suggests that astronomers build a special gamma-ray detector to detect gamma rays produced during the proton-proton chain in the core of the Sun, just like they built a neutrino detector. Explain why this would be a fruitless effort.arrow_forwardWhy is fission not an important energy source in the Sun?arrow_forwardWhat conditions are required before proton-proton chain fusion can start in the Sun?arrow_forward
- Do neutrinos have mass? Describe how the answer to this question has changed over time and why.arrow_forwardWhat do measurements of the number of neutrinos emitted by the Sun tell us about conditions deep in the solar interior?arrow_forwardExplain why some solar shock waves are thought to die out at heliocentric distances of 3-5 R. How can we observe this?arrow_forward
- a) At solar maximum sunspots might cover up to 0.4% of the total area of the Sun. If the sunspots have a temperature of 3800 K and the surrounding photosphere has a temperature of 6000 K, calculate the fractional change (as a percentage) in the luminosity due to the presence of the sunspots. b) A star of the same stellar class as the Sun is observed regularly over many years, and a time series of its bolometric apparent magnitude is collected. What would be the signal in this time series which indicated that the star had a magnetic dynamo similar to the Sun? Briefly describe two or three possible sources of other signals which could confuse the interpretation of the data.arrow_forwardA loop of gas following the magnetic field lines between sunspots' poles is called a what? \arrow_forwardW S 7 What is the ultimate source of energy that makes the Sun shine? nuclear fusion O mechanical to thermal energy conversion O Kelvin-Helmholtz contraction O radioactivity O chemical burning # 3 e d с $ A t 4 f do in % 5 t D.O Σ Oll 6 0 T & 7 h ▸ u 8arrow_forward
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