EBK LOOSE-LEAF VERSION OF UNIVERSE
11th Edition
ISBN: 9781319227975
Author: KAUFMANN
Publisher: VST
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 21, Problem 37Q
To determine
The time it will take for two neutron stars to collide with each other. It is given that the distance between two stars is in the range of
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solutionStudents have asked these similar questions
velocity curve for a double line
spectroscopic binary is shown in the sketch.
The system is viewed edge-on, i.e., with an
inclination angle of i 90°, so that the
maximum possible Doppler shifts for this
system are observed.
400
SPo
= , Ain i
300
200
l0o = v Ain i
100
-100
-200
-300
400
0 1 2 3 4
10
Time (days)
Find the speed of star 2 in km/s.
Doppler Velocity
(2esu)
Problem Set on Binary Systems:
1.Consider two stars in orbit about a mutual center of mass. If a1 is the semimajor axis of
the orbit of star of mass m, and a, is the semimajor axis of the orbit of star of mass m2,
prove that the semimajor axis of the orbit of the reduced mass is given by a = a, + a2.
points)
Time left 1:45:56
A star has initially a radius of 680000000 m and a period of rotation about its axis of 33 days.
Eventually it changes into a neutron star with a radius of only 45000 m and a period of 0.3 s.
Assuming that the mass has not changed, find
Assume a star has the shape of a sphere.
(Suggestion: do it with formula first, then put the numbers in)
[Recommended time : 5-8 minutes]
(a) the ratio of initial to final angular momentum (Li/Lf)
Oa. 2.17E+15
Ob. 24
Oc. 0.0416
Od. 4.61E-16
(b) the ratio of initial to final kinetic energy
Oa. 4.85E-23
Ob. 396000
Oc. 2.53E-6
Od. 2.06E+22
Chapter 21 Solutions
EBK LOOSE-LEAF VERSION OF UNIVERSE
Ch. 21 - Prob. 1CCCh. 21 - Prob. 2CCCh. 21 - Prob. 3CCCh. 21 - Prob. 4CCCh. 21 - Prob. 5CCCh. 21 - Prob. 6CCCh. 21 - Prob. 7CCCh. 21 - Prob. 8CCCh. 21 - Prob. 9CCCh. 21 - Prob. 10CC
Ch. 21 - Prob. 11CCCh. 21 - Prob. 12CCCh. 21 - Prob. 13CCCh. 21 - Prob. 14CCCh. 21 - Prob. 15CCCh. 21 - Prob. 16CCCh. 21 - Prob. 17CCCh. 21 - Prob. 18CCCh. 21 - Prob. 19CCCh. 21 - Prob. 20CCCh. 21 - Prob. 21CCCh. 21 - Prob. 1QCh. 21 - Prob. 2QCh. 21 - Prob. 3QCh. 21 - Prob. 4QCh. 21 - Prob. 5QCh. 21 - Prob. 6QCh. 21 - Prob. 7QCh. 21 - Prob. 8QCh. 21 - Prob. 9QCh. 21 - Prob. 10QCh. 21 - Prob. 11QCh. 21 - Prob. 12QCh. 21 - Prob. 13QCh. 21 - Prob. 14QCh. 21 - Prob. 15QCh. 21 - Prob. 16QCh. 21 - Prob. 17QCh. 21 - Prob. 18QCh. 21 - Prob. 19QCh. 21 - Prob. 20QCh. 21 - Prob. 21QCh. 21 - Prob. 22QCh. 21 - Prob. 23QCh. 21 - Prob. 24QCh. 21 - Prob. 25QCh. 21 - Prob. 26QCh. 21 - Prob. 27QCh. 21 - Prob. 28QCh. 21 - Prob. 29QCh. 21 - Prob. 30QCh. 21 - Prob. 31QCh. 21 - Prob. 32QCh. 21 - Prob. 33QCh. 21 - Prob. 34QCh. 21 - Prob. 35QCh. 21 - Prob. 36QCh. 21 - Prob. 37QCh. 21 - Prob. 38QCh. 21 - Prob. 39QCh. 21 - Prob. 40QCh. 21 - Prob. 41QCh. 21 - Prob. 42QCh. 21 - Prob. 43QCh. 21 - Prob. 44QCh. 21 - Prob. 45QCh. 21 - Prob. 46QCh. 21 - Prob. 47QCh. 21 - Prob. 48QCh. 21 - Prob. 49QCh. 21 - Prob. 50QCh. 21 - Prob. 51QCh. 21 - Prob. 52QCh. 21 - Prob. 53QCh. 21 - Prob. 54QCh. 21 - Prob. 55QCh. 21 - Prob. 56QCh. 21 - Prob. 57QCh. 21 - Prob. 58QCh. 21 - Prob. 59QCh. 21 - Prob. 60QCh. 21 - Prob. 61QCh. 21 - Prob. 62QCh. 21 - Prob. 63QCh. 21 - Prob. 64QCh. 21 - Prob. 65QCh. 21 - Prob. 66QCh. 21 - Prob. 67QCh. 21 - Prob. 68QCh. 21 - Prob. 69QCh. 21 - Prob. 70QCh. 21 - Prob. 71QCh. 21 - Prob. 72QCh. 21 - Prob. 73QCh. 21 - Prob. 74QCh. 21 - Prob. 75QCh. 21 - Prob. 85QCh. 21 - Prob. 86Q
Knowledge Booster
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- What characteristics must a binary star have to be a good candidate for a black hole? Why is each of these characteristics important?arrow_forwardvelocity curve for a double line spectroscopic binary is shown in the sketch. The system is viewed edge-on, i.e., with an inclination angle of i = 90°, so that the maximum possible Doppler shifts for this system are observed. 400 300 So = U, Ani 200 t0 = v Ain i 100 -100 -200 -300 400 O 1 2 3 1 s 1 8: 10 Time (days) Find the orbital period of this binary in days. Doppler Velocity (krn/sec)arrow_forwardAn astronomical image shows two objects that have the same apparent magnitude, i.e., the same brightness. However, spectroscopic follow up observations indicate that while one is a star that is within our galaxy, at a distance dgal away, and has the same luminosity as the Sun, the other is a quasar and has 100x the luminosity of the entire Milky Way galaxy. What is the distance to the quasar? (You may assume, for this rough calculation, that the Milky Way has 1011 stars and that they all have the luminosity as the Sun.) Give your response in Mpc. Value: dgal = 49 pcarrow_forward
- A visual binary has a parallax of 0.4 arcseconds, a maximum separation a = 6.0 arcseconds, and an orbital period P = 80 years. What is the total mass of the binary system in units of Mo, assuming a circular orbit?arrow_forwardA star has initially a radius of 660000000 m and a period of rotation about its axis of 34 days. Eventually it changes into a neutron star with a radius of only 35000 m and a period of 0.2 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) Oa. 5.22E+15 Ob. 24.2 Oc. 0.0413 Od. 1.91E-16 (b) the ratio of initial to final kinetic energy Oa. 1.3E-23 Activate V Go to Setting Ob. 607000 Oc. 1.65E-6 e here to searcharrow_forwardA star has initially a radius of 780000000 m and a period of rotation about its axis of 22 days. Eventually it changes into a neutron star with a radius of only 25000 m and a period of 0.1 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) a. 1.85E+16 b. 51.2 c. 0.0195 d. 5.4E-17 (b) the ratio of initial to final kinetic energy a. 2.84E-24 b. 371000 c. 2.69E-6 d. 3.52E+23arrow_forward
- Q1 (oints): A0620-00 is an X-ray binary system, there is a normal star and a compact object. For the normal star the radial orbital velocity is 457 km s and for the compact object it is 43 km s1.They have an orbital period of 0.3226 day. Calculate the mass function.arrow_forwardA star has initially a radius of 640000000 m and a period of rotation about its axis of 20 days. Eventually it changes into a neutron star with a radius of only 50000 m and a period of 0.2 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) Oa. 1.42E+15 Ob. 19 Oc. 0.0527 Od. 7.06E-16 (b) the ratio of initial to final kinetic energy Oa. 8.18E-23 Ob. 456000 Oc. 2.19E-6 Od. 1.22E+22 52%arrow_forwardA star has initially a radius of 680000000 m and a period of rotation about its axis of 26 days. Eventually it changes into a neutron star with a radius of only 40000 m and a period of 0.2 s. Assuming that the mass has not changed, find Assume a star has the shape of a sphere. (Suggestion: do it with formula first, then put the numbers in) [Recommended time : 5-8 minutes] (a) the ratio of initial to final angular momentum (Li/Lf) Oa. 3.25E+15 Ob. 25.7 Oc. 0.0389 Od. 3.08E-16 (b) the ratio of initial to final kinetic energy Oa. 2.74E-23 Ob. 437000 Cc. 2.29E-6 FUJITSUarrow_forward
- From the light and velocity curves of an eclipsing spectroscopic binary star system, it is determined that the orbital period is 6.31 yr and the maximum radial velocities of stars A and B are 5.4 km/s and 22.4 km/s, respectively. Furthermore, the time period between first contact and minimum light (tp-ta) is 0.58 d and the length of the primary minimum (tc-tb) is 0.64 d. From this information, assuming circular orbits, find: a) the ratio of stellar masses. b) the sum of masses (i ~ 90°). c) the individual masses. d) the individual radii.arrow_forwardA 1.5 M neutron star and a 0.7 M white dwarf have been found orbiting each other with a period of 10 minutes. What is their average separation? Convert your answer to units of the Sun's radius, which is 0.0047 AU.arrow_forwardA cepheid star is located at a distance of 24.8kpc from the Earth and has an apparent visual magnitude of 13.3. Determine its pulsation period in days. Consider the following expression of the Leavitt relation My -2.78 log Pdays - 1.35, where My is the absolute visual magnitude and Pdays the pulsation period in days to 2 decimal places.arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
- Foundations of Astronomy (MindTap Course List)PhysicsISBN:9781337399920Author:Michael A. Seeds, Dana BackmanPublisher:Cengage LearningStars and Galaxies (MindTap Course List)PhysicsISBN:9781337399944Author:Michael A. SeedsPublisher:Cengage LearningAstronomyPhysicsISBN:9781938168284Author:Andrew Fraknoi; David Morrison; Sidney C. WolffPublisher:OpenStax
Foundations of Astronomy (MindTap Course List)
Physics
ISBN:9781337399920
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Stars and Galaxies (MindTap Course List)
Physics
ISBN:9781337399944
Author:Michael A. Seeds
Publisher:Cengage Learning
Astronomy
Physics
ISBN:9781938168284
Author:Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher:OpenStax