Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 8, Problem 43Q
To determine
The part that is wrong in the statement, “the newly discovered galaxy, with three large planets orbiting a star known as Upsilon Andromedae, is
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Check out a sample textbook solutionStudents have asked these similar questions
1) There is a one earth mass planet orbiting an M5 star of 0.2 Mo and luminosity 1x10-2 Lo-
A) How close does the planet need to be to the star in order to receive the same amount of energy
as the Earth receives from the sun?
B) What is the orbital period of the planet at this distance?
C) What is the magnitude of the radial velocity perturbation of the star?
D) If the system is edge on to us, would we be likely to detect this planet using the radial
velocity method?
Exoplanet orbital period (b)
For the system pictured in the previous problem (and using data given there), suppose that the star
has a mass of 0.025 solar masses, and the planet's mass is very small in comparison. Compute the
planet's orbit period. Assume the orbit is circular with a radius given by the distance listed in the
figure. Express your answer in years.
[Hint: this is a mildly challenging problem that requires plugging into a single formula but using
multiple unit conversions. You will need to use Kepler's 3rd law in its **general** form (not the
simplified form that is only applicable to objects orbiting our Sun). You will need to look up the
value of the constant G. Convert solar masses to kg, AU to m, and everything else to base Sl units;
find the period in seconds; then convert seconds to years.]
The Tully-Fischer method relies on being able to relate the mass of a galaxy to its rotation velocity. Stars in the outer-most regions of the Milky Way galaxy, located at a distance of 50 kpc from the galactic centre, are observed to orbit at a speed vrot = 250 km s−1. Using Kepler’s 3rd Law, determine the mass in the Milky Way that lies interior to 50 kpc. Express your answer in units of the Solar mass.
Chapter 8 Solutions
Universe: Stars And Galaxies
Ch. 8 - Prob. 1QCh. 8 - Prob. 2QCh. 8 - Prob. 3QCh. 8 - Prob. 4QCh. 8 - Prob. 5QCh. 8 - Prob. 6QCh. 8 - Prob. 7QCh. 8 - Prob. 8QCh. 8 - Prob. 9QCh. 8 - Prob. 10Q
Ch. 8 - Prob. 11QCh. 8 - Prob. 12QCh. 8 - Prob. 13QCh. 8 - Prob. 14QCh. 8 - Prob. 15QCh. 8 - Prob. 16QCh. 8 - Prob. 17QCh. 8 - Prob. 18QCh. 8 - Prob. 19QCh. 8 - Prob. 20QCh. 8 - Prob. 21QCh. 8 - Prob. 22QCh. 8 - Prob. 23QCh. 8 - Prob. 24QCh. 8 - Prob. 25QCh. 8 - Prob. 26QCh. 8 - Prob. 27QCh. 8 - Prob. 28QCh. 8 - Prob. 29QCh. 8 - Prob. 30QCh. 8 - Prob. 31QCh. 8 - Prob. 32QCh. 8 - Prob. 33QCh. 8 - Prob. 34QCh. 8 - Prob. 35QCh. 8 - Prob. 36QCh. 8 - Prob. 37QCh. 8 - Prob. 38QCh. 8 - Prob. 39QCh. 8 - Prob. 40QCh. 8 - Prob. 41QCh. 8 - Prob. 42QCh. 8 - Prob. 43QCh. 8 - Prob. 44QCh. 8 - Prob. 45QCh. 8 - Prob. 46QCh. 8 - Prob. 47QCh. 8 - Prob. 48QCh. 8 - Prob. 49QCh. 8 - Prob. 50QCh. 8 - Prob. 51QCh. 8 - Prob. 52Q
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- Our Solar System is about 8.3 kpc from the centre of our galaxy. Using Newton's Universal Gravitation Law and Kepler's Third Law, calculate the approximate mass of our Milky Way if we know that the orbital velocity of the Sun around the centre of the galaxy is 225 km/s. (Hint: Use the formula for orbital velocity: v = GM -and problem , r -11 m3 Note: G is the Universal Gravitation Constant, G 6.67 × 10 kg s2' 1 kpс 1000 рс аnd 1 рс 3.1 x 1016 m. Also, pay attention to units!!! – i.e. orbital m3 velocity is in km/s and the universal gravitation constant is in kgs2 а) 8.7 х 1035 b) 2.0 x 1041kg c) 2.0 × 1030 d) 6.0 × 1024 kg kg kgarrow_forwardYou are at a weekly meeting of your Astronomy Club. The club members are excited because access is now available to real-time data on light intensity from the star at the center of another planetary system. The plane of the system is parallel to the direction from the system toward the Earth, so it is possible to detect transits: a planet passes between the Earth and the star of the system, so that the light from the star dims slightly. The planets of this system are very close to their parent star and revolve very rapidly. Planet X in this system has a period of 4.00 Earth days! As you graph the incoming data from the star as it appears on a computer, you see the dip in light intensity. You make a printout of the graph of light intensity versus time and compare it to the graph from 4.00 days ago. The latest graph shows a difference. The time interval from the beginning of the dimming of the light from the star to the return to full brightness took much longer than it did during the…arrow_forwarda) Calculate the period of the solar system's orbit around the Milky Way. Assume that we are 8.5 kpc from the galactic center and assume that the mass of the Milky Way interior to our orbit is ~ 10¹¹ solar masses. Alpha Centauri is a multiple star system only 1.34 parsecs away. The apparent magnitudes of the two main stars are: a Cen A: my = +0.01; a Cen B: my = +1.33. b) Calculate the ratio of the flux we receive in the V filter from a Cen A to the flux we receive from a Cen B. c) Calculate the absolute magnitude My of a Cen B.arrow_forward
- Using high resolution adaptive optical techniques, observations of a nearby (9.5 pc) cool star of mass 0.2 solar masses indicate the presence of a small rocky exoplanet in a circular orbit with a radius of 0.01 arcseconds. Using Kepler's Laws, estimate the period of the exoplanet's orbit in days. select units Aarrow_forwardDetermining the orbit of the two stars of Kepler-34, also called A and B. These two stars together are called a binary. A) Assume that star A has a mass of 1 solar mass and star B also has a mass of 1 solar mass. The semi major axis is 0.23 AU and the eccentricty is 0.53. What is the orbital period of the stellar A-B binary in days? Ignore the (much less massive) planet and focus on the orbit of the binary. B) Now let's consider the orbit of the planet, called "b". Since the planet orbits some distance away from the stars, it is an acceptable approximation to pretend like the stellar binary is like a single star with a mass that is the sum of the masses of stars A and B and that the mass of planet "b" is very small, calculate the semi-major axis in AU of the planet's orbit with a period of 289 days. (note: I think for this problem you are supposed to use Newton's version of Kepler's third law P2= 4π2/G(M1-M2)x a3 but, I'm not sure if that's the right thing to do). 1 solar mass= 2 x…arrow_forward(Astronomy) Binary Pulsar. Part A: Use the orbital period 27 min for the binary pulsar (two neutron stars orbit each other) to find the orbital separation of the pair in AU and solar radii. Assume a neutron star's mass is 3 solar masses. (Hints: Use the version of Kepler's third law for binary stars.) Part B: Is this system orbiting closer or further than Mercury is to the Sun?arrow_forward
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