Alleviating the $H_0$ tension through new interacting dark energy model in light of DESI DR2

The $H_0$ tension has become one of the most significant challenges in modern cosmology. The recent DESI DR2 data has shown a significant preference for dynamical dark energy, yet this has further exacerbated the $H_0$ tension. In this work, we explore the potential of new interacting dark energy models ($\tilde{\mathrm{\Lambda }}$CDM and $e\tilde{\mathrm{\Lambda }}$CDM) to alleviate the $H_0$ tension. We perform observational constraints using the latest baryon acoustic oscillation data from DESI DR2, cosmic microwave background (CMB) data from Planck and Atacama Cosmology Telescop, and type Ia supernova data from DESY5 and PantheonPlus, as well as the SH0ES data. From our analysis, we observe the dynamical scale parameter of the cosmological constant, ${\delta }_{\mathrm{\Lambda }}=-0.410_{-0.120}^{+0.140}$, in the $e\tilde{\mathrm{\Lambda }}$CDM model using the CMB+DESI+SH0ES data, which deviates from $\mathrm{\Lambda }$CDM at the $3.2\sigma$ level. Due to the anti-correlation between ${\delta }_{\mathrm{\Lambda }}$ and $H_0$, a negative ${\delta }_{\mathrm{\Lambda }}$ results in a higher inferred $H_0$. Consequently, we obtain $H_0=71.90\pm 1.00\mathrm{k}\mathrm{m}{\mathrm{s}}^{-1}\mathrm{M}\mathrm{p}{\mathrm{c}}^{-1}$, reducing the $H_0$ tension to $0.8\sigma$. Even without SH0ES, the CMB+DESI data alone still alleviate the $H_0$ tension to $1.7\sigma$. Overall, the $e\tilde{\mathrm{\Lambda }}$CDM model not only deviates from the $\mathrm{\Lambda }$CDM model but also demonstrates a significant capability to alleviate the $H_0$ tension.