We briefly review the recent results of constraining neutrino mass in dynamical dark energy models using cosmological observations and summarize the findings .
( i ) In dynamical dark energy models , compared to \Lambda CDM , the upper limit of \sum m _ { \nu } can become larger and can also become smaller .
In the cases of phantom and early phantom ( i.e. , the quintom evolving from w < -1 to w > -1 ) , the constraint on \sum m _ { \nu } becomes looser ; but in the cases of quintessence and early quintessence ( i.e. , the quintom evolving from w > -1 to w < -1 ) , the constraint on \sum m _ { \nu } becomes tighter .
( ii ) In the holographic dark energy ( HDE ) model , the tightest constraint on \sum m _ { \nu } , i.e. , \sum m _ { \nu } < 0.105 eV , is obtained , which is almost equal to the lower limit of \sum m _ { \nu } of IH case .
Thus , it is of great interest to find that the future neutrino oscillation experiments would potentially offer a possible falsifying scheme for the HDE model .
( iii ) The mass splitting of neutrinos can influence the cosmological fits .
We find that the NH case fits the current observations slightly better than the IH case , although the difference of \chi ^ { 2 } of the two cases is still not significant enough to definitely distinguish the neutrino mass hierarchy .