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Astrology: An accretion disk of a protostar takes mass from the ___________ and gives mass to _________

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the co te on Pictor. The 270 TOI System TOI 270 c Earth 365-day orbit $1 AU from Sun Habitable 5.7-day orbit 0.05 AU $2.4 Earth radii Largest in system 59 F, 15 C 300 F, 150 C TOI 270 TOI 270 d M3-type dwarf star TOI 270 b $11.4-day orbit 0.07 AU 3.4-day orbit 2.1 Earth radii 0.03 AU Temperate 1.25 Earth radii Likely rocky 150 F. 67 C 490 F. 254 C Figure taken from https://exoplanets.nasa.gov/news/1593/tess-scores-hat-trick-with-3-new-worlds/ What makes the TOI-270 system particularly interesting is that the three exoplanets detected this far (there may be more) have sizes comparable to the Earth. Compare the orbital period of TOI 270 c and TOI 270 d. For every revolution that TOI 270 d makes around the host star TOI 270, how many revolutions does TOI 270 c make?
The rate at which a nebular cloud rotates increases as the cloud collapses to form systems of stars and planets. Consider a small segment of a nebular cloud with a mass m of 1.9 x 102" kg, tangential velocity vinitial equal to 6.8 km s-1 located at an orbital distance rinitial = 2.5 x 10* km. After the cloud collapses, the same small segment is located at an orbital distance rinal = 3.2 x 10° km. Calculate the change of the rotational velocity, Ao, for the cloud segment, assuming perfectly circular orbits. Perform your work and report your solution using two significant figures. Δω- 16605 rad s-!
(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?
(Astronomy) PSR1913+16 Problem II. Using only the Figure, what are the maximum radial velocities as found from the redshift and blueshift, respectively? Note: redshifts have positive radial velocities values in the figure, whereas blueshifts have negative radial velocity values. (Answer in km/s)
The star HD 69830's mass is 1.7 ✕ 1030 kg, its radius is 6.3 ✕ 105 km, and it has a rotational period of approximately 35 days. If HD 69830 should collapse into a white dwarf of radius 7.8 ✕ 103 km, what would its period (in s) be if no mass were ejected and a sphere of uniform density can model HD 69830 both before and after?
One way that astronomers detect planets outside of our solar system (called exoplanets) is commonly referred to as the radial velocity method. This relies on the __________ ___________ to cause shifts in the spectral lines of stars as the stars perform tiny orbits around the center of mass of the host star and its orbiting planets. Those tiny orbits cause the stars to periodically (and therefore predictably) move closer to and further away from our solar system. Luckily, this method only relies on the motion of the star; its physical distance from us does not impact the resulting shifts.
A gravitational dead zone is found between two hyper giant stars, HG A and HG B, 34 million km from HG A. It is known that the mass of B is 25 x the mass of A. Determine the distance between the two stars in millions of km.
A 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%
Consider a neutron star as a very dense sphere of matter. Assuming that the star has a mass of 1*(mass of sun) and a radius of 0.05*(radius of sun), then how much would a 85.1 kg person weigh on the surface of this star? (enter your answer in Newtons). See the test reference sheet for applicable constants. HINT: Remember what we learned about the force of gravity and the gravitational field (Ch. 13 of the textbook)
(Astronomy) Neutron Star Escape Velocity. What is the escape velocity at the surface of a 2.80-solar-mass neutron star that has a typical radius for this type of star? Express your answer in units of km/s.
where did the 50 x 10^-3 come from and how did you get the math of -7.5
The rate at which a nebular cloud rotates increases as the cloud collapses to form systems of stars and planets. Consider a small segment of a nebular cloud with a mass m of 1.9 x 102" kg, tangential velocity vinitial equal to 6.8 km s-1 located at an orbital distance rinitial = 2.5 x 10* km. After the cloud collapses, the same small segment is located at an orbital distance rinal = 3.2 x 10° km. Calculate the change of the rotational velocity, A», for the cloud segment, assuming perfectly circular orbits. Perform your work and report your solution using two significant figures. Δω- rad s- %3D