Remanent magnetism at Mars
Remanent magnetism at Mars
复制标题
火星的剩磁
DOI：
10.1029/gl015i008p00737
复制
发表时间：
1988
影响因子：
5.2
通讯作者：
N. Ness
中科院分区：
文献类型：
--
作者：
S. Curtis;N. Ness
我们表明，一个强有力的情况下，可以作出的内在磁场的发电机起源火星在其历史的早期。典型的赤道磁场强度为0.01-0.1高斯。早期的发电机活动已不复存在，但可能存在一个重要的反射磁场。一个高度非偶极磁场可能是由于表面的反磁化。因此，剩余磁化可能在火星太阳风相互作用中发挥重要作用，而金星的表面温度高于居里点。火星与金星太阳风相互作用的异常特征可以在此基础上得到解释。
We show that a strong case can be made for an intrinsic magnetic field of dynamo origin for Mars earlier in its history. The typical equatorial magnetic field intensity would have been ∼ 0.01-0.1 Gauss. The earlier dynamo activity is no longer extant, but a significant remanent magnetic field may exist. A highly non-dipole magnetic field could result from the remanent magnetization of the surface. Remanent magnetization may thus play an important role in the Mars solar wind interactions in contrast to Venus with its surface temperatures above the Curie point. The anomalous characteristics of Mars’ solar wind interaction compared to that of Venus may be explicable on this basis.