THE UBV(RI)(C) COLORS OF THE SUN

Autor(es)

Ramirez, I. ^{[1, 2]} ; Michel, R. ^[3] ; Sefako, R. ^[4] ; Tucci Maia, M. ^[5] ; Schuster, W. J. ^[3] ; van Wyk, F. ^[4] ; Melendez, J. ^[6] ; Casagrande, L. ^[7] ; Castilho, B. V. ^[8]

Afiliação do(s) autor(es)

^[1] Univ Texas Austin, Dept Astron, Austin, TX 78712 - USA

^[2] Univ Texas Austin, McDonald Observ, Austin, TX 78712 - USA

^[3] Univ Nacl Autonoma Mexico, Observ Astron Nacl, Ensenada 22800, Baja California - Mexico

^[4] S African Astron Observ, ZA-7935 Cape Town - South Africa

^[5] Univ Fed Itajuba, UNIFEI, DFQ Inst Ciencias Exatas, Itajuba, MG - Brazil

^[6] Univ Sao Paulo, Dept Astron IAG USP, BR-05508900 Sao Paulo - Brazil

^[7] Max Planck Inst Astrophys, D-85741 Garching - Germany

^[8] Lab Nacl Astrofis MCT, BR-37504364 Itajuba, MG - Brazil

• Tipo de documento: Artigo Científico
• Fonte: ASTROPHYSICAL JOURNAL; v. 752, n. 1 JUN 10 2012.
• Citações Web of Science: 46

Resumo

Photometric data in the UBV(RI)(C) system have been acquired for 80 solar analog stars for which we have previously derived highly precise atmospheric parameters T-eff, log g, and {[}Fe/H] using high-resolution, high signal-to-noise ratio spectra. UBV and (RI)(C) data for 46 and 76 of these stars, respectively, are published for the first time. Combining our data with those from the literature, colors in the UBV(RI) C system, with similar or equal to 0.01 mag precision, are now available for 112 solar analogs. Multiple linear regression is used to derive the solar colors from these photometric data and the spectroscopically derived T-eff, log g, and {[}Fe/H] values. To minimize the impact of systematic errors in the model-dependent atmospheric parameters, we use only the data for the 10 stars that most closely resemble our Sun, i.e., the solar twins, and derive the following solar colors: (B - V)(circle dot) = 0.653 +/- 0.005, (U - B)(circle dot) = 0.166 +/- 0.022, (V - R)(circle dot) = 0.352 +/- 0.007, and (V - I)(circle dot) = 0.702 +/- 0.010. These colors are consistent, within the 1 sigma errors, with those derived using the entire sample of 112 solar analogs. We also derive the solar colors using the relation between spectral-line-depth ratios and observed stellar colors, i.e., with a completely model-independent approach, and without restricting the analysis to solar twins. We find (B - V)(circle dot) = 0.653 +/- 0.003, (U - B)(circle dot) = 0.158 +/- 0.009, (V - R)(circle dot) = 0.356 +/- 0.003, and (V - I)(circle dot) = 0.701 +/- 0.003, in excellent agreement with the model-dependent analysis. (AU)

• Processo FAPESP: 10/17510-3 - Influência da formação de planetas na composição química de estrelas do tipo solar
• Beneficiário: Jorge Luis Melendez Moreno
• Modalidade de apoio: Auxílio à Pesquisa - Regular