X-ray observations provide a key tool for exploring the properties of galactic coronae and their formation processes .
In an earlier paper , we have presented a Chandra data analysis of the coronae of 53 nearby highly-inclined disc galaxies .
Here we study the correlation of the X-ray measurements of the coronae with other galaxy properties and compare the results with those obtained for elliptical galaxies .
A good correlation is present between the coronal luminosity ( L _ { X } ) and the star formation rate ( SFR ) .
But we find a better correlation between L _ { X } and the total SN mechanical energy input rate ( \dot { E } _ { SN } ) , including the expected contribution from both core collapsed ( CC ) and Type Ia SNe .
The X-ray radiation efficiency ( \eta \equiv L _ { X } / \dot { E } _ { SN } ) of the coronae has a mean value of \sim 0.4 \% with an rms of 0.50 \pm 0.06 ~ { } dex . \eta further correlates with M _ { TF } / M _ { * } ( M _ { TF } is the total baryon mass measured from the rotation velocity and the Tully-Fisher relation , M _ { * } is the stellar mass measured from the K-band luminosity ) and the CC SN rate surface density ( F _ { SN ( CC ) } , in units of SN~ { } yr ^ { -1 } ~ { } kpc ^ { -2 } ) , which can be characterized as : \eta = ( 0.41 _ { -0.12 } ^ { +0.13 } \% ) M _ { TF } / M _ { * } and \eta = ( 1.4 \pm 0.5 \% ) F _ { SN ( CC ) } ^ { - ( 0.29 \pm 0.11 ) } .
These correlations reflect the roles that played by the gravitational mass and energetic feedback concentrations of the galaxies in determining their X-ray radiation efficiency .
The characteristic temperature ( T _ { X } ) of the coronal gas shows little dependence on the total or specific SFR , the cold gas content , or L _ { X } .
The coronae of disc galaxies tend to be more X-ray luminous , hotter , and lower in the Fe/O abundance ratio than those of elliptical ones of similar masses .
Early-type non-starburst disc galaxies tend to be more Fe-rich , while starburst ones have a roughly constant abundance ratio of { Fe / O } \sim 0.36 \pm 0.12 ~ { } solar .
Our results are consistent with the coronal gas being mainly provided by stellar feedback in a galaxy stellar mass range of \sim 10 ^ { 8.7 - 11 } ~ { } M _ { \odot } .
In addition , processes such as charge exchange at cool/hot gas interfaces , as well as various other environmental effects , are also needed to explain the diversity of the observed coronal X-ray properties .