 The time a star spends on the main sequence depends primarily on the amount of fuel it has and the rate at which it fuses it . The Sun 's is expected to live 10 billion ( 1010 ) years . Massive stars consume their fuel very rapidly and are short @-@ lived . Low mass stars consume their fuel very slowly . Stars less massive than 0 @.@ 25 M ☉ , called red dwarfs , are able to fuse nearly all of their mass while stars of about 1 M ☉ can only fuse about 10 % of their mass . The combination of their slow fuel @-@ consumption and relatively large usable fuel supply allows low mass stars to last about one trillion ( 1012 ) years ; the most extreme of 0 @.@ 08 M ☉ ) will last for about 12 trillion years . Red dwarfs become hotter and more luminous as they accumulate helium . When they eventually run out of hydrogen , they contract into a white dwarf and decline in temperature . However , since the lifespan of such stars is greater than the current age of the universe ( 13 @.@ 8 billion years ) , no stars under about 0 @.@ 85 M ☉ are expected to have moved off the main sequence . 
 The time a star <a href='uninflect' title='1'><mark>spends</mark></a> on the main sequence <a href='uninflect' title='2'><mark>depends</mark></a> primarily on the amount of fuel it <a href='uninflect' title='3'><mark>has</mark></a> and the rate at which it <a href='uninflect' title='4'><mark>fuses</mark></a> it . The Sun <a href='null_genetive' title='5'><mark>'s</mark></a>is expected to live 10 billion ( 1010 ) years . Massive stars consume their fuel very rapidly and <a href='drop_aux' title='6'><mark>are</mark></a>short @-@ lived . Low mass stars consume their fuel very slowly . Stars less massive than 0 @.@ 25 M ☉ , called red dwarfs , <a href='drop_aux' title='7'><mark>are</mark></a>able to fuse nearly all of their mass while stars of about 1 M ☉ can only fuse about 10 % of their mass . The combination of their slow fuel @-@ consumption and relatively large usable fuel supply <a href='uninflect' title='8'><mark>allows</mark></a> low mass stars to last about one trillion ( 1012 ) years ; the most extreme of 0 @.@ 08 M ☉ ) will last for about 12 trillion years . Red dwarfs <a href='uninflect' title='9'><mark>become</mark></a> hotter and more luminous as they accumulate helium . When they eventually run out of hydrogen , they contract into a white dwarf and decline in temperature . However , since the lifespan of such stars <a href='drop_aux' title='10'><mark>is</mark></a>greater than the current age of the universe ( 13 @.@ 8 billion years ) , no stars under about 0 @.@ 85 M ☉ are expected to <a href='been_done' title='11'><mark>have</mark></a> moved off the main sequence . 
The time a star spend on the main sequence depend primarily on da amount of fuel it have and the rate at which it fuse it . The Sun  is expected to live 10 billion ( 1010 ) years . Massive stars consume their fuel very rapidly and short @-@ lived . Low mass stars consume their fuel very slowly . Stars less massive den 0 @.@ 25 M ☉ , called red dwarfs , able to fuse nearly all of their mass while stars of abt 1 M ☉ can only fuse about 10 % of their mass . The combination of their slow fuel @-@ consumption and relatively large usable fuel supply allow low mass stars to last abboutne trillion ( 1012 ) years ; the most extreme of 0 @.@ 08 M ☉ ) will last fa abobou trillion years . Red dwarfs became hotter and more luminous as they accumulate helium . When they eventually run outt of hydrogen , they contract into a white dwarf and decline in temperature . However , since the lifespan of such stars greater than the current age of the universe ( 13 @.@ 8 billion years ) , no stars under about 0 @.@ 85 M ☉ are expected to done moved off the main sequence .