 The magnetic field of a star is generated within regions of the interior where convective circulation occurs . This movement of conductive plasma functions like a dynamo , wherein the movement of elecrical charges induce magnetic fields , as does a mechanical dynamo . Those magnetic fields have a great range that extend throughout and beyond the star . The strength of the magnetic field varies with the mass and composition of the star , and the amount of magnetic surface activity depends upon the star 's rate of rotation . This surface activity produces starspots , which are regions of strong magnetic fields and lower than normal surface temperatures . Coronal loops are arching magnetic field flux lines that rise from a star 's surface into the star 's outer atmosphere , its corona . The coronal loops can be seen due to the plasma they conduct along their length . Stellar flares are bursts of high @-@ energy particles that are emitted due to the same magnetic activity . 
 The magnetic field of a star is generated within regions of the interior where convective circulation <a href='uninflect' title='1'><mark>occurs</mark></a> . This movement of conductive plasma functions like a dynamo , wherein the movement of elecrical charges induce magnetic fields , as <a href='uninflect' title='2'><mark>does</mark></a> a mechanical dynamo . Those magnetic fields <a href='got' title='3'><mark>have</mark></a> a great range <a href='null_relcl' title='4'><mark>that</mark></a>extend throughout and beyond the star . The strength of the magnetic field <a href='uninflect' title='5'><mark>varies</mark></a> with the mass and composition of the star , and the amount of magnetic surface activity <a href='uninflect' title='6'><mark>depends</mark></a> upon the star <a href='null_genetive' title='7'><mark>'s</mark></a>rate of rotation . This surface activity <a href='uninflect' title='8'><mark>produces</mark></a> starspots , which <a href='drop_aux' title='9'><mark>are</mark></a>regions of strong magnetic fields and lower than normal surface temperatures . Coronal loops are arching magnetic field flux lines <a href='null_relcl' title='10'><mark>that</mark></a>rise from a star <a href='null_genetive' title='11'><mark>'s</mark></a>surface into the star <a href='null_genetive' title='12'><mark>'s</mark></a>outer atmosphere , its corona . The coronal loops can be seen due to the plasma they conduct along their length . Stellar flares <a href='drop_aux' title='13'><mark>are</mark></a>bursts of high @-@ energy particles <a href='null_relcl' title='14'><mark>that</mark></a>are emitted due to the same magnetic activity . 
Da magnetic field of a star is generated within regions of the interior where convective circulation occur . This movement of conductive plasma functions like a dynamo , wherein the movement of elecrical charges induce magnetic fields , as do a mechanical dynamo . Those magnetic fields got a great range extend throughout and beyond the star . The strength of the magnetic field vary with the mass and composition of tdastar , and thdamount of magnetic surface activity depend upon thedaar  rate of rotation . This surface activity produce starspots , which regions of strong magnetic fields and lower den normal surface temperatures . Coronal loops r arching magnetic field flux lines rise from a star  surface into the dar  outer atmosphere , its corona . The coronal loops can b seen due to the pdama they conduct along their length . Stellar flares bursts of high @-@ energy particles are emitted due to the same magnetic activity .