Newly born massive magnetars are generally considered to be produced by binary neutron star ( NS ) mergers , which could give rise to short gamma-ray bursts ( SGRBs ) .
The strong magnetic fields and fast rotation of these magnetars make them promising sources for gravitational wave ( GW ) detection using ground based GW interferometers .
Based on the observed masses of Galactic NS-NS binaries , by assuming different equations of state ( EOSs ) of dense matter , we investigate the stochastic gravitational wave background ( SGWB ) produced by an ensemble of newly born massive magnetars .
The massive magnetar formation rate is estimated through : ( i ) the SGRB formation rate ( hereafter entitled as MFR1 ) ; ( ii ) the NS-NS merger rate ( hereafter entitled as MFR2 ) .
We find that for massive magnetars with masses M _ { mg } = 2.4743 M _ { \odot } , if EOS CDDM2 is assumed , the resultant SGWBs may be detected by the future Einstein Telescope ( ET ) even for MFR1 with minimal local formation rate , and for MFR2 with a local merger rate \dot { \rho } _ { c } ^ { o } ( 0 ) \lesssim 10 { Mpc } ^ { -3 } { Myr } ^ { -1 } .
However , if EOS BSk21 is assumed , the SGWB may be detectable by the ET for MFR1 with the maximal local formation rate .
Moreover , the background spectra show cutoffs at about 350 Hz in the case of EOS BSk21 , and at 124 Hz for CDDM2 , respectively .
We suggest that if the cutoff at \sim 100 Hz in the background spectrum from massive magnetars could be detected , then the quark star EOS CDDM2 seems to be favorable .
Moreover , the EOSs , which present relatively small TOV maximum masses , would be excluded .