The following lists of stars in order from least density to greatest density are giant, main sequence star, white dwarf, neutron star. Aside from neutron star being the densest star, it is also the smallest star compared to the giant star, as its name implied.
A.) the gravitational pull of the Sun
B.) the interstellar dust attracting heat away from the protosun
C.) the process of nuclear fusion
D.) the nebular cloud condensing
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Which type of reaction is C2H2011 - 12C + 11H202
O synthesis
decomposition
O oxidation
combustion
Answer:
A
Explanation:
synthesis decompostion
Answer:
Decompositon
Explanation:
Answer:
High crater density is associated with older surfaces.
Explanation:
b. False
Answer:
True
Explanation:
In a binary system with a main-sequence star and a brown dwarf, we can determine their masses by analyzing their radial velocity curve and measuring the Doppler shifts of their spectral lines. Kepler's law can then be used to calculate the sum of their masses.
The question is about a binary system containing a main-sequence star and a brown dwarf. We can determine the masses of the stars in a spectroscopic binary by analyzing their radial velocity curve. By measuring the Doppler shifts of the spectral lines, we can calculate the orbital speed of each star and use Kepler's law to calculate the sum of their masses.
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The orbital speed and separation of a binary system composed of a main-sequence star and a brown dwarf can be utilized to infer their respective masses. This is accomplished by studying the Doppler effect from the spectral lines of the system and applying Kepler's third law. Greater mass is found to exhibit slower orbital speed.
The main-sequence star and the brown dwarf form a binary system with an orbital period of 1 year and an average separation of 1 Astronomical Unit (AU). The Doppler shifts of the spectral lines from the main-sequence star and the brown dwarf indicate that the orbital speed of the brown dwarf in the system is 22 times greater than that of the main-sequence star.
We can estimate the masses of the stars in this binary system using the formula based on Newton's reformulation of Kepler's third law: D³ = (M₁ + M₂)P², where D represents the semimajor axis in AU and P represent the period in years. From this, we can calculate the sum of the masses of the two stars. Given the difference in orbital speeds, the main-sequence star has a higher mass to result in a slower speed, and the brown dwarf has a smaller mass to result in the higher speed.
In conclusion, by analyzing the radial velocity curve and using Kepler's third law, we can estimate the masses of the stars in a binary system.
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