hite dwarf stars are produced by the collapse of regular stars, such as our sun, toward the end of their normal life. Suppose a star initially has the same mass as our sun and the same radius as that of the sun. Suppose further that it collapses into a white dwarf with a radius of 5000km. If the initial period of the star is the same 27 day period of our sun, what is the resulting period of the white dw

hite dwarf stars are produced by the collapse of regular stars, such as our sun, toward the end of their normal life. Suppose a star initially has the same mass as our sun and the same radius as that of the sun. Suppose further that it collapses into a white dwarf with a radius of 5000km. If the initial period of the star is the same 27 day period of our sun, what is the resulting period of the white dw

Similar questions

A. Use the definition of the center of mass to determine the maximum “wobble” velocity of a star of mass M caused by a planet of mass m orbiting at a distance r from the star with a period T. B. Thanks to Kepler, we know that the mass, period, and distance of an orbiting object are actually related. Use Newton’s version of Kepler’s Third Law to determine the maximum “wobble” velocity in terms of M, m, and r.
A planet has been discovered orbiting the sun-like star HD 209458. From the period and velocity measured by the Doppler method, its mass was calculated to be 0.69 times that of Jupiter. The plane of the planet's orbit is edge-on and it has been observed to transit across the face of the star. The light from the star was seen to drop by 1.7% when the planet's disc lay fully within that of the star which has a radius of 8 × 10°km. Assuming that the brightness of the star is constant across the observed face, estimate the diameter of the planet and hence it density in comparison with that of Jupiter which has a radius of 7.1 × 10ʻkm. 3.
Around 2.5 centuries ago, several physicists of the time came up with the notion of a dark star. This was a star so dense, with so much gravity, that not even light could escape. The calculations used Newtonian mechanics. In class, we calculated the escape speed from the surface of the earth or the distance from the sun, and the mass of the planet or star. Here, the process is partially reversed. Calculate the dark star radius from the mass of the star and the escape speed. Answer in kilometers. c = 3*108 m/s M = 2.4*1030 kg G = 2/3 * 10-10 N*m2/kg2
Nothing can escape the event horizon of a black hole, not even light. You can think of the event horizon as being the distance from a black hole at which the escape speed is the speed of light, 3.00 ×× 1088 m/sm/s, making all escape impossible. What is the radius of the event horizon for a black hole with a mass 7.5 times the mass of the sun? This distance is called the Schwarzschild radius.?
Nothing can escape the event horizon of a black hole, not even light. You can think of the event horizon as being the distance from a black hole at which the escape speed is the speed of light, 3.00×10^8 m/s, making all escape impossible. What is the radius of the event horizon for a black hole with a mass 3.5 times the mass of the sun?
As a star ages, it is believed to undergo a variety of changes. One of the last phases of a star's life is to gravitationally collapse into a black hole. If suppose our Sun would end up a Black hole, what will happen to the orbit of the planets of the solar system? (Assuming that the planets are not affected by the evolving stages of the Sun prior to becoming a black hole and noting that for calculation of gravitational force of attraction, the distance being considered is from center to center of the two bodies). Justify your answer.
Around 2.5 centuries ago, several physicists of the time came up with the notion of a dark star. This was a star so dense, with so much gravity, that not even light could escape. The calculations used Newtonian mechanics. In class, we calculated the escape speed from the surface of the earth or the distance from the sun, and the mass of the planet or star. Here, the process is partially reversed. Calculate the dark star radius from the mass of the star and the escape speed. Answer in kilometers. c = 3*108 m/s M = 3.2*1030 kg G = 2/3 * 10-10 N*m2/kg2
Neptune has a mass of 1.0 × 1026 kg and is 4.5 × 10⁹ km from the Sun with an orbital period of 177.5 years. Planetesimals in the outer primordial solar system 4.5 billion years ago coalesced into Neptune over hundreds of millions of years. If the primordial disk that evolved into our present day solar system had a radius of 10¹1 km and if the matter that made up these planetesimals that later became Neptune was spread out evenly on the edges of it, what was the orbital period of the outer edges of the primordial disk? Express your answer rounded to the nearest year, and be sure not to do any rounding before expressing your final answer. P = years
Hunting a black hole. Observations of the light from a certain star indicate that it is part of a binary (two-star) system. This visible star has moves in a circle of radius r1 and has orbital period T. Variations in the brightness of nearby stars suggest that the unseen companion moves in a circle of radius r2 (see the figure). Find the approximate masses (a) m1 of the visible star and (b) m2 of the dark star. Express your answer in terms of r1, r2, T, and G. I asked this question before and recieved an incorrect answer, so I'm asking again.
Plaskett's binary system consists of two stars that revolve in a circular orbit about a center of mass midway between them. This statement implies that the masses of the two stars are equal (see figure below). Assume the orbital speed of each star is V = 240 km/s and the orbital period of each is 12.1 days. Find the mass M of each star. (For comparison, the mass of our Sun is 1.99 x 1030 kg.) solar masses XCM M
A meteoroid is moving towards a planet. It has mass m = 0.54×109 kg and speed v1 = 4.7×107 m/s at distance R1 = 1.6×107 m from the center of the planet. The radius of the planet is R = 0.78×107 m. The mass of the planet is M = 5.6×1025kg. There is no air around the planet. a)Enter an expression for the total energy E of the meteoroid at R, the surface of the planet, in terms of defined quantities and v, the meteoroid’s speed when it reaches the planet’s surface. Select from the variables below to write your expression. Note that all variables may not be required.α, β, θ, d, g, G, h, m, M, P, R, R1, t, v, v1 b)Enter an expression for v, the meteoroid’s speed at the planet’s surface, in terms of G, M, v1, R1, and R. c)Calculate the value of v in meters per second.
A star with mass M and radius R collides head-on with another star of mass ¾*M and radius 4/5*R, and they coalesce to form a new start at rest whose radius is 6/5*R. Assume that initially the colliding stars had angular velocities with opposite directions but the same magnitude w. What is the magnitude and direction of the final’s stars angular velocity? (Express the magnitude as a fraction of w.)