摘要
In this work, a computer optimization model has been developed that allows one to load the initial data of observations of supernovae 1a into a table and, in simple steps, by searching for the best fit between observations and theory, obtain the values of the parameters of cosmological models. The optimization is carried out assuming that the absolute magnitude of supernovae is not constant, but evolves with time. It is assumed that the dependence of the absolute magnitude on the redshift is linear: M = M( z = 0) + ε<sub>c </sub>z, where ε<sub>c</sub> is the evolution coefficient of the absolute magnitude of type 1a supernovae. In the case of a flat universe ( Ω<sub>M</sub> + Ω<sub>Λ</sub> = 1 ), the best fit between theory and observation is εc </sub>= 0.304. In this case, for the cosmological parameters we obtain Ω<sub>Λ</sub> = 0.000, Ω<sub>M</sub><sub></sub> =1.000. Naturally, this result exactly coincides with the simulation result for the model with zero cosmological constant ( εc</sub> = 0.304, q<sub>0</sub> = 0.500 ). Within the framework of the ΛCDM model, without restriction on space curvature ( Ω<sub>M</sub> + Ω<sub>Λ</sub>+ Ω<sub>K</sub><sub></sub> = 1 ), we obtain the following values: εc</sub> </sub>= 0.304, ΩΛ</sub> = 0.000, ΩM </sub>= 1.000, Ω<sub>K</sub></sub></sub></sub> =0.000. Those, this case also leads to a flat model of the Universe ( Ω<sub>K</sub><sub></sub></sub></sub> =0.000 ). In this work, the critical influence of the absolute magnitude M of type 1a supernovae on the cosmological parameters is also shown. In particular, it was found that a change in this value by only 0.4<sup>m </sup>(from -19.11 to -18.71) leads to a change in the parameters from ΩΛ</sub> = 0.7 and ΩM</sub></sub> = 0.3 to ΩΛ</sub> = 0 and ΩM</sub> =1.
In this work, a computer optimization model has been developed that allows one to load the initial data of observations of supernovae 1a into a table and, in simple steps, by searching for the best fit between observations and theory, obtain the values of the parameters of cosmological models. The optimization is carried out assuming that the absolute magnitude of supernovae is not constant, but evolves with time. It is assumed that the dependence of the absolute magnitude on the redshift is linear: M = M( z = 0) + ε<sub>c </sub>z, where ε<sub>c</sub> is the evolution coefficient of the absolute magnitude of type 1a supernovae. In the case of a flat universe ( Ω<sub>M</sub> + Ω<sub>Λ</sub> = 1 ), the best fit between theory and observation is εc </sub>= 0.304. In this case, for the cosmological parameters we obtain Ω<sub>Λ</sub> = 0.000, Ω<sub>M</sub><sub></sub> =1.000. Naturally, this result exactly coincides with the simulation result for the model with zero cosmological constant ( εc</sub> = 0.304, q<sub>0</sub> = 0.500 ). Within the framework of the ΛCDM model, without restriction on space curvature ( Ω<sub>M</sub> + Ω<sub>Λ</sub>+ Ω<sub>K</sub><sub></sub> = 1 ), we obtain the following values: εc</sub> </sub>= 0.304, ΩΛ</sub> = 0.000, ΩM </sub>= 1.000, Ω<sub>K</sub></sub></sub></sub> =0.000. Those, this case also leads to a flat model of the Universe ( Ω<sub>K</sub><sub></sub></sub></sub> =0.000 ). In this work, the critical influence of the absolute magnitude M of type 1a supernovae on the cosmological parameters is also shown. In particular, it was found that a change in this value by only 0.4<sup>m </sup>(from -19.11 to -18.71) leads to a change in the parameters from ΩΛ</sub> = 0.7 and ΩM</sub></sub> = 0.3 to ΩΛ</sub> = 0 and ΩM</sub> =1.
作者
Abraham P. Mahtessian
Garen S. Karapetian
Martik A. Hovhannisyan
Lazar A. Mahtessian
Abraham P. Mahtessian;Garen S. Karapetian;Martik A. Hovhannisyan;Lazar A. Mahtessian(Byurakan Astrophysical Observatory after V. Ambartsumian, NAS of the Republic of Armenia, Byurakan, Republic of Armenia;Institute of Applied Problems of Physics, NAS of the Republic of Armenia 25 Hrachya Nersissian Str., Yerevan, Republic of Armenia)
