A star must have at least a certain mass, the exact number depends on the star's composition, in order for gravity to be strong enough to sustain fusion of hydrogen-1 at the core. Bodies just under that mass are known as brown dwarfs, which have a mass somewhere between the largest gas giants and the smallest stars.
No they about the same. The mass of a proton is 1.6726x10^-27kg or 1.0073U and the mass of a neutron is 1.6749x10^-27kg or 1.0087U.
In the UK it is 60mph for cars and motorcycles, 40mph for goods vehicles. Unless a lower speed limit is in force. This is assuming it is a single carriageway road.
Towards a region of lower pressure.
it's a protostar
The majority of the mass in the solar system is contained in the sun, which is a star, not a planet. The Majority of the mass in the solar system outside of the sun is contained in the planet Jupiter.
It's because a gas cloud has to have a critical mass in order to generate enough temperature to start the nuclear processes that enable the star to radiate heat and light.
The Sun is a medium mass star on the main sequence.
FALSE FALSE
There is an upper limit to the mass of neutron stars because if the neutron star is too massive, neutrons would be crushed by the gravity of the neutron star, and the neutron star would collapse into a black hole.
The difference between a star and a planet with such a mass is kind of fuzzy. I would say it is a brown dwarf - a very small and dim star. The smallest known star is currently OGLE-TR-122b with a mass of 0.09 Msun. THey think the lower limit for a star to have fusion occur is about 0.08 Msun. So, an object with 0.017 Msun would be a planet.
The Chandrasekhar limit describes the maximum stable mass of a highly compressed type of star called a white dwarf - a collapsed remnant of a star towards the end of its life cycle. This mass limit is about 1.44 times the mass of the sun; above this mass, gravitational force is calculated to overcome the outward pressure and thus precipitate further collapse, for example, into a neutron star. If the neutron star is of sufficient mass it may yet again collapse further, into more exotic states including possibly a black hole. Note that the mass limit of a neutron star (the Tollman-Oppenheimer-Volkoff limit) of around 3-4 solar masses is separate and distinct from the Chandrasekhar limit - you might say that the Chandrasekhar limit is just one of the mass limits along the stellar remnant's evolution into a black hole.
The white dwarf (which is made mostly of carbon) suddenly detonates carbon fusion and this creates a white dwarf supernova explosion.
Yes, there are limits for stars - limits to lower and upper mass, longevity, size, etc. Given the mass of the universe a limit for the number of extant stars would also exist. During stellar collapse at end of a star's life there are some well-studied limits answering to degeneracy pressure, like the Chandresekhar limit, the Oppenheimer-Volkoff limit, etc., which prevent further collapse until a certain mass limit is exceeded (perhaps the last limit being quark degeneracy pressure before further collapse into a black hole). For further examination of a given limit, the limit in question would need to be identified.
It is, but at twice our suns mass, Sirius A is on the limit, of being an intimidate mass star. Sirius A will have a life cycle similar to that of our own star which is a low mass star, but burns hotter. Sirius B is a companion white dwarf star with a mass of around the same as our sun. Previously, it was thought to have been a star with a mass of around 5 times that of our sun, burning out more quickly than Sirius A.
Hopefully you mean the Chandrasekhar Limit or Chandra Limit (Named after the Indian born Astrophysicist bearing that name) which states the maximum mass of a White Dwarf Star. If the Star exceeds this limit, then gravity will overcome pressure within the Star and it will collapse into a Neutron Star or Black Hole. See link for further information
The lower mass limit is a subject of debate; it might be somewhere around 13 times the Jupiter mass.
A low-mass star never gets hot enough in the core to fuse helium into carbon.