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By Aniket Sule

This can be a compilation of difficulties from the overseas Olympiad in Astronomy and
Astrophysics (2007-2012).

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I10 - T08 - B) 4. What is the minimum diameter of a telescope, observing in the visible and near ultraviolet bands and located at one of the Lagrangian points L4 or L5 s of the Sun-Earth system, in order to be able to detect the Earth’s wobbling relative to the ecliptic plane caused by the gravitational action of the Moon? (I12 - T12 B) 5. The coordinates of the components of Visual Binary star µ Sco as on the August 28, 2008 are given in the table below. 30s h δ (Dec) −12◦ 30′30′′ −12◦ 32′41′′ 24 Optics and Detectors The stars are observed using Zeiss refractor telescope at the Bosscha Observatory whose aperture and focal length are 600 mm and 10,780 mm respectively.

I09 - T12 - C) 19. A pulsar, located 1000 pc far from Earth and 10,000 times more luminous than our Sun, emits radiation only from its two opposite poles, creating an homogeneous emission beam shaped as double cone with opening angle α = 4◦ . Assuming the angle between the rotation axis and the emission axis is 30◦ , and assuming a random orientation of the pulsar beams in relation to an observer on Earth, what is the probability of detecting the pulses? In case we can see it, what is the apparent bolometric magnitude of the pulsar?

I10 - T14 - D) 12. On average, the visual diameter of the Moon is slightly less than that of the Sun, so the frequency of annular solar eclipses is slightly higher than total solar eclipses. 5 minutes. Here, the longest duration is the time interval from the second contact to the third contact. Suppose we count the occurrences of both types of solar eclipses for a very long time, estimate the ratio of the occurrences of annular solar eclipses and total solar eclipses. 0549. Count all hybrid eclipses as annular eclipses.

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A Problem book in Astronomy and Astrophysics by Aniket Sule

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