恒星轨迹是在颜色空间中反映恒星颜色等信息的重要形式，在现代天文学研究中有着广泛的应用。恒星的颜色长期以来一直用于估算恒星金属丰度等恒星参数。本文使用经过SCR方法修正后的SDSS stripe 82标准星表v4.2，数据深度和广度较之前有明显提升。将其与 LAMOST DR7等星表交叉，得到包含SDSS星等、LAMOST恒星参数和GAIA距离信息的数据。我们分别得到了g-i颜色在0.55-1.2、Fe/H在-2.5-0.3范围的巨星样本和0.3-1.9、Fe/H在-2.5-0.5范围的矮星样本。巨星与矮星的颜色内禀宽度都很小，至多只有几个毫星等。金属丰度增加会使得u-g和g-r颜色增加，r-i颜色和i-z颜色减小。并且金属丰度越大，金属丰度变化引起的颜色变化越明显。本文给出了巨星与矮星金属丰度与颜色之间的拟合公式，确定了巨星和矮星颜色的内禀宽度，并在最后尝试探究了主序拐点和亚巨星的金属丰度与颜色之间的关系。

Stellar locus is an important form to reflect the color and other information of stellar in color space, which is widely used in modern astronomical research. The color of stellar has long been used to estimate the metallicity of stars. This paper uses the SDSS stripe 82 standard star catalog v4.2 calibrated by SCR method , whose data precision has been significantly improved than before. SDSS magnitudes, LAMOST stellar parameters and Gaia distance information are obtained by crossing it with LAMOST DR7 catalog and others. Then we obtained giant samples with g-i color in the range of 0.55-1.2 and Fe / H in the range of - 2.5-0.3 and dwarf samples with g-i color in the range of 0.3-1.9 and Fe / H in the range of - 2.5-0.5. The intrinsic width of the color of giants and dwarfs is quite narrow, only a few mmag at maximun. The increase of metallicity will cause the increase of u-g and g-r, and the decrease of r-i and i-z. And the greater the metal abundance, the more obvious the color change caused by metallicity. This paper gives the fitting formula between the metallicity and color of giants and dwarfs, determines the intrinsic width of the color of giants and dwarfs. Finally ,we attempts to explore the relationship between the metallicity and color for turning points of the main sequence and subgiants.