Giant Magnetic Dipole Resonance (GMDR) related to spin-flip transitions between major shells . The peak cross section is normalized to the $E1$ strength function at $E_{\gamma} = 7$ MeV as described in Ref. [@RIPL], while the width and the peak position is determined from systematics [@RIPL]. With such a parameterization the $M1$ contribution to the total RSF remains low compared to the $E1$ contribution.

The GLO-lo, GLO-up1 and GLO-up2 models are shown together with experimental data on $^{93-98}$Mo in Fig. \[fig02\]. For $^{98}$Mo, also the GLO model with $E_n = 1$ MeV is displayed. It is seen that both the GLO-up1 and the GLO-up2 models give reasonable agreement with data at all energies, while GLO-lo fails to describe the low-energy region.

![image](MoRSF_GLO.pdf)

In the following section, the impact of the upbend structure is estimated by comparing the above-mentioned models (GLO-up1, GLO-up2, and GLO-lo) and the original and widely used $T$-dependent GLO model.

Results {#sect_res}
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We now perform the calculation of $(n,\gamma)$ cross-sections and astrophysical rates with the code TALYS [@TALYS; @go08b] in order to study the impact the upbend structure might have on the radiative neutron capture for stable as well as neutron-rich nuclei. By default, all calculations are 