On the main sequence, a 30 solar mass star loses a larger proportion of its mass (30 to 28 Msun) than a 1 solar mass star (1 to 0.9 Msun) does. Over their whole lifetime? The total change in mass for 30 Msun star is 30Msun to 6Msun, for the 1 Msun star it changes 1Msun to 0.5Msun. D. Wien’s Law Using the data table on the Star in a Box website and your knowledge of Wien’s Law, complete the following table. HINT: Wien’s Law: λmax T = 2.898 x10-3 m.K Mass of Star Main Sequence Main Sequence Region of EM (Msun) Temperature (K) λmax (μm) spectrum 1 5,788 0.501 Visible (green) 2 7,332 0.395 Visible (violet) 6 14,655 0.198 Ultraviolet 10 21,622 0.134 Ultraviolet 20 26,872 0.107 Ultraviolet 30 27,765 0.104 Ultraviolet 40 27,492 0.105 Ultraviolet E. Stefan-Boltzmann Law Using the data table on the Star in a Box, complete the following table. HINTS: Assume all the stars are spherical. You will need to convert some of the values into SI units. Lsun = 3.8 x 1026 W Rsun = 3 x 108 m Stefan’s Law: Main Main Main Main Mass of Main Surface Area of Sequence Sequence Sequence Sequence Star Sequence Main Sequence Temperature Radius Luminosity Luminosity (Msun) Radius (m) Star (m2) (K) (Rsun) (Lsun) (W) 1 5,788 1.69 0.507x109 32.23 x1018 2.82 1.07 x1027 2 7,332 3.71 1.11 x109 1.54 x1019 1,163.03 4.42 x1029 6 14,655 7.48 2.24 x109 6.31 x1019 2,286.13 8.69 x1029 10 21,622 9.34 2.80 x109 9.85 x1019 16,873.30 6.41 x1030
On the main sequence, a 30 solar mass star loses a larger proportion of its mass (30 to 28 Msun) than a 1 solar mass star (1 to 0.9 Msun) does. Over their whole lifetime? The total change in mass for 30 Msun star is 30Msun to 6Msun, for the 1 Msun star it changes 1Msun to 0.5Msun. D. Wien’s Law Using the data table on the Star in a Box website and your knowledge of Wien’s Law, complete the following table. HINT: Wien’s Law: λmax T = 2.898 x10-3 m.K Mass of Star (Msun) Main Sequence Temperature (K) Main Sequence λmax (μm) Region of EM spectrum 1 5,788 0.501 Visible (green) 2 7,332 0.395 Visible (violet) 6 14,655 0.198 Ultraviolet 10 21,622 0.134 Ultraviolet 20 26,872 0.107 Ultraviolet 30 27,765 0.104 Ultraviolet 40 27,492 0.105 Ultraviolet E. Stefan-Boltzmann Law Using the data table on the Star in a Box, complete the following table. HINTS: Assume all the stars are spherical. You will need to convert some of the values into SI units. Lsun = 3.8 x 1026 W Rsun = 3 x 108 m Stefan’s Law: Mass of Star (Msun) Main Sequence Temperature (K) Main Sequence Radius (Rsun) Main Sequence Radius (m) Surface Area of Main Sequence Star (m2) Main Sequence Luminosity (Lsun) Main Sequence Luminosity (W) 1 5,788 1.69 0.507x109 32.23 x1018 2.82 1.07 x1027 2 7,332 3.71 1.11 x109 1.54 x1019 1,163.03 4.42 x1029 6 14,655 7.48 2.24 x109 6.31 x1019 2,286.13 8.69 x1029 10 21,622 9.34 2.80 x109 9.85 x1019 16,873.30 6.41 x1030
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