41. It is also undergoing strong mass loss with the outer layers of the star no longer gravitationally bound. 42. It also shows H ? emission lines with P Cygni profiles, indicating mass loss through a powerful stellar wind. 43. Ordinary supergiants lack the strong H emission and broadened spectral lines that indicate rapid mass loss in the hypergiants. 44. In the TGA trace of calcium oxalate monohydrate, the first mass loss corresponds to loss of water of hydration. 45. This is about 5 times greater than the observed mass loss in Greenland but still in the same ballpark. 46. Only the very lowest metallicity population III stars will reach this stage of their life with little mass loss . 47. The mass loss from the collision will not be detectable before the radiated energy passes beyond the observers position. 48. This weight loss and mass loss would happen as the box was cooled by this process, to room temperature. 49. The second mass loss corresponds to decomposition of dehydrated calcium oxalate to calcium carbonate and carbon monoxide and carbon dioxide. 50. At such a rate of mass loss , the star probably has only another one million to three million years to live.
