We construct a relativistic model for the newly discovered millisecond pulsar PSR J0514-4002A located in the globular cluster NGC 1851 (Ridolfi et al. in MNRAS 490:3860, 2019) by using Tolman VII spacetime. We have obtained central density (\(\rho _{0}\)), central pressure (\(p_{0}\)), probable radius, compactness (u) and surface redshift (\(Z_\mathrm{s}\)) of the above-mentioned newly discovered millisecond pulsar, which is very much consistent with reported data. Equation of state of the millisecond pulsar has come out as stiff in nature which is physically acceptable. Not even that our proposed model can analyze most of the millisecond pulsars having masses up to \(1.51 M_{\odot }\).

我们使用Tolman VII时空为位于球状星团NGC 1851中的新发现的毫秒脉冲星PSR J0514-4002A建立了相对论模型（Ridolfi等人在MNRAS 490：3860，2019）。我们获得了中心密度（\（\ rho _ {0} \）），中心压力（\（p_ {0} \）），可能的半径，密实度（u）和表面红移（\（Z_ \ mathrm {s}） \））是上述新发现的毫秒脉冲星，与报告的数据非常一致。毫秒脉冲星的状态方程本质上是刚性的，在物理上是可以接受的。甚至我们提出的模型也无法分析质量最高达\（1.51 M _ {\ odot} \）的大多数毫秒脉冲星。