使用CMOS相机进行流星色度测量
Meteor colorimetry with CMOS cameras
摘要：
本文介绍了我们的方法来量化流星的特性，如温度，化学成分，和其他。我们正在使用一种基于色度学的新方法。我们分析了Mike Hankey在2012年获得的狮子座流星6230的图像。分析了流星体尾迹的时间特征。为了确定流星的特点，我们使用的“调整技术”结合入侵的模拟模型。流星的前身是一个重900公斤、速度为36.5公里/秒的物体。流星体在约4.6秒的时间内在约29公里的高度达到压力临界值，剩余质量约为20公斤，剩余速度约为28公里/秒。就在这时，一颗陨石爆炸，毁灭。我们使用的流星多色光变曲线显示从数码单反相机图像中的RGB颜色标准。我们从RGB颜色系统切换到Johnson的RVB颜色系统，引入颜色校正。这使人们能够确定流星辐射的颜色特征。我们正在使用一种基于色度学的新方法。BGR三光束光变曲线的比色法可以识别最亮的谱线。我们的方法的基础上比色法允许直接测量的流星轨迹的温度。我们发现了流星体作为绝对黑体辐射的轨迹的一部分。R/G和B/G光变曲线比率允许使用RGB滤光器的透射曲线来识别发射谱线的波长。在轨道末端，流星体的辐射线为Ca II H，K 393，397 nm，Fe I 382，405 nm，Mg I 517 nm，Na I 589 nm，以及大气O I 779 nm。
英文摘要：
This article describes our approach to quantifying the characteristics of meteors such as temperature, chemical composition, and others. We are using a new approach based on colourimetry. We analyze an image of Leonid meteor-6230 obtained by Mike Hankey in 2012. Analysis of the temporal features of the meteoroid trail is performed. For determining the meteor characteristics we use the "tuning technique" in combination with a simulation model of intrusion. The progenitor of the meteor was found as an object weighing 900 kg at a speed of 36.5 km/s. The meteoroid reached a critical value of the pressure at an altitude of about 29 km in a time of about 4.6 sec with a residual mass of about 20 kg, and a residual speed of about 28 km/s. At this moment, a meteoroid exploded and destroyed. We use the meteor multicolour light curves revealed from a DSLR image in the RGB colour standard. We switch from the RGB colour system to Johnson's RVB colour system introducing colour corrections. This allows one to determine the colour characteristics of the meteor radiation. We are using a new approach based on colourimetry. Colourimetry of BGR three-beam light curves allows the identification of the brightest spectral lines. Our approach based on colourimetry allows direct measurements of temperature in the meteor trail. We find a part of the trajectory where the meteoroid radiates as an absolutely black body. The R/G and B/G light curves ratio allow one to identify the wavelengths of the emission lines using the transmission curves of the RGB filters. At the end of the trajectory, the meteoroid radiates in the lines Ca II H, K 393, 397 nm, Fe I 382, 405 nm, Mg I 517 nm, Na I 589 nm, as well as atmospheric O I 779 nm.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
