论文标题
来自Gaia DR3宽二进制的太阳能星的重力红移
The gravitational redshift of solar-type stars from Gaia DR3 wide binaries
论文作者
论文摘要
从重力势能逃脱的光遭受的红移，其大小与电势深度成正比。这种“重力红移”很容易在诸如白色矮人之类的密集恒星中可测量，但弱得多，并且已经在主要序列恒星中逃避了明确的检测。我表明，在宽二进制恒星的成分的Gaia Dr3径向速度（RV）中，该效果是可直接测量的。在$ \ sim的样本中，$ 500宽的二进制文件，其中包含太阳能主序列明星和红色巨人或红色团块伴侣，这家巨人的明显RV平均为$ 0.49 \ pm 0.02 \，\，\，\ rm \ rm km km km km km \，s^{ - 1} $比主序列明星。这主要归功于巨人的重力较弱，并且与一般相对性预期的价值相当良好。
Light escaping from a gravitational potential suffers a redshift with magnitude proportional to the depth of the potential. This "gravitational redshift" is easily measurable in dense stars such as white dwarfs, but is much weaker and has evaded unambiguous detection in main-sequence stars. I show that the effect is directly measurable in the Gaia DR3 radial velocities (RVs) of the components of wide binary stars. In a sample of $\sim$500 wide binaries containing a solar-type main-sequence star and a red giant or red clump companion, the apparent RV of the giant is on average $0.49 \pm 0.02 \,\, \rm km\,s^{-1}$ lower than that of the main-sequence star. This owes primarily to the giants' weaker gravitational fields and is in reasonably good agreement with the value expected from general relativity.
