Solar Spectral Irradiance (SSI) from CODET model and their relation with Earth s upper atmosphere

Transcription

1 Solar Spectral Irradiance (SSI) from CODET model and their relation with Earth s upper atmosphere Jenny Marcela Rodríguez Gómez PhD in Space Geophysics (INPE) Collaborators: Luis Eduardo Antunes Vieira Alisson Dal Lago Judith Palacios April

2 Earth s atmosphere Sun s dynamics Solar Wind ARs Electromagnetic emission in different wavelengths: SSI and TSI HMI data CMEs Coronal Holes (CHs)

3 Solar Spectral Irradiance (SSI) and Earth s atmosphere Ionosphere EUV - Satellite communication-gps Stratosphere The SSI variation at EUV wavelengths has important consequences for the Earth s upper atmosphere because the SSI is completely absorbed into the tenuous layers above the stratosphere (Schöll et al. 2016; Fontenla et al. 2017) EUV - chemistry

4 COronal DEnsity and Temperature model The COronal DEnsity and Temperature (CODET) model is based on the assumption that the variation of the irradiance and plasma parameters is due to the evolution of the solar magnetic field. Ingredients Flux transport model Density and temperature model Emission model We do not use MHD approximation

5 COronal DEnsity and Temperature model Search the best fit parameters Rodríguez Gómez et al. 2018

6 Solar magnetic field data MDI data HMI data

7 Flux transport model of Schrijver (2003) MDI and HMI data are assimilated into the flux transport model to describe the dynamics of the solar photosphere The model is sampled every six hours from 1996 July 1 These data are then used as boundary conditions for a series of potential field sourcesurface (PFSS) Rodríguez Gómez et al. 2018

8 Potential Field Source Surface (PFSS) model Current-free corona Synoptic maps of the photospheric magnetic field Extrapolate the line-of-sight surface magnetic field from 1.0Rsun to 2.5Rsun

9 Density and temperature profiles description Density profile Bth function Temperature profile

10 Density and temperature profiles description Density profile Model parameters Bth function Temperature profile

11 Emission Model 1AU Based on the contribution function G(λ,T), instrumental response R(λ), spectral resolution dλ, different distance along of line-of sight ds Chianti atomic database 8.0, ionization equilibrium (Mazzotta et al. 1998) and coronal abundances (Meyer 1985) model

12 Emission Model 1AU The intensity I is the full-disc average intensity measured at Earth from an emission line, where D = 1AU

13 Optimization algorithm- Genetic algorithm pikaia Biological processes - the natural selection. Charbonneau (1995) The population of individuals (parameters) is chosen at random range They are surveyed to determine their goodness-of-fit A new generation of individuals is generated Their characteristics are passed on to the next generation

14 Optimization algorithm- Genetic algorithm pikaia Rodríguez Gómez et al. 2018

15 CODET Model Parameters I model SSI from CODET I obs SSI from TIMED/SEE Rodríguez Gómez et al. 2018

16 CODET Model Parameters The characteristics evaluated in each case were (1) goodness-of-fit between SSI from TIMED/SEE and modeled data; (2) electron density and temperature profiles according to observational and model descriptions (Billings 1966; Withbroe 1988; Aschwanden 2005; Golub & Pasachoff 2009; Habbal et al. 2010; Fontenla et al. 2014)

17 Main Results Solar Spectral Irradiance (SSI) in EUV band at 19.5 nm and 21.5 nm during the solar cycle 23 and 24 Emission maps through the solar atmosphere Temperature and density profiles during the solar cycle 23 and 24

18 Density and Temperature profiles through the solar atmosphere Temperature profile (left panel) and density profile (right panel) through the solar atmosphere on Dec. 15 (2001); specifically from R = 1Rsun to R = 2.5Rsun, for the parameter combinations shown in Table 1

19 The transition region demarcates the boundary where the chromospheric temperature increases and the density drops

20 SSI - EUV band Ciclo 23 solar Ciclo 24 solar Rodríguez Gómez et al. 2018

21 Rodríguez Gómez et al. 2018

22 Next steps The reconstruction of the solar spectral irradiance in near-real time Flux transport model (sampled < six hours) Include UV and other wavelengths Use in: Ionosphere models Climate models More details about the model are available in Rodríguez Gómez et al ApJ

23 Thank you!