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<img src='content_image/332018.jpg'>

that third inflection point on the spectrum is far from the observable region. If we could observe the second inflection, we can deduce the reheating temperature. 

Note that the spectrum depends on Gµ via the overall factor ( Gµ ) $^{2}$. Therefore, when we vary the value on Gµ , the spectrum only moves upward or downward, and its shape (e.g., the position of bending) does not change. This situation is different from the case of GWs from cosmic string loops. In the case of cosmic string loops, since different values of Gµ give different values of lifetime of loops, the resultant spectral shape is different [4, 5]. 

Let us discuss detectability of this GW background. We have to see whether GWs from kinks exceeds not only thresholds of various experiments but also GWs from other source. The spectrum of GWs from loops was discussed in [4–9], and the contribution of loops to 

