Spectroscopic Observations of Ten Galactic Wolf-Rayet Stars at Bosscha Observatory:Determination of Stellar Parameters and Mass-loss Rates  

作　　者：Hakim Luthfi Malasan Bakuh Danang Setyo Budi 

机构地区：[1]Department of Astronomy,Faculty of Mathematics and Natural Sciences,Institut Teknologi Bandung,Bandung 40132,Indonesia [2]Bosscha Observatory,Institut Teknologi Bandung,Lembang 40391,Indonesia [3]Master Program in Astronomy,Faculty of Mathematics and Natural Sciences,Institut Teknologi Bandung,Jl.Ganesha No.10,Bandung 40132,Indonesia

出　　处：《Research in Astronomy and Astrophysics》2024年第9期7-27,共21页天文和天体物理学研究（英文版）

基　　金：supported through HLM’s Program Penelitian Pengabdian Masyarakat ITB(P2MI)Astronomy Division,FMIPA ITB grant 2022-2023;Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts。

摘　　要：We present optical spectra of 10 Galactic Wolf-Rayet(WR)stars that consist of five WN and five WC stars.The optical observation was conducted using a low-resolution spectrograph NEO-R1000(λ/Δλ~1000)at GAO-ITB RTS(27.94 cm,F/10.0),Bosscha Observatory,Lembang.We implemented stellar atmosphere Postdam Wolf-Rayet(PoWR)grid modeling to derive stellar parameters.The normalized optical spectrum can be used to find the best model from the available PoWR grid,then we could derive stellar temperature and transformation radius.To derive luminosity,stellar radius and color excess,we conducted a Spectral Energy Distribution(SED)analysis with additional data on the near-ultraviolet spectrum from the International Ultraviolet Explorer(IUE)database,and UBV and 2MASS JHK broadband filter data.Additional analysis to derive asymptotic terminal wind velocity was conducted from the P-Cygni profile analysis of the high-resolution IUE ultraviolet spectrum.With previously derived parameters,we could determine the mass loss rate of the WR stars.Furthermore,we compared our results with previous work that used PoWR code and the differences are not more than 20%.We conclude that the PoWR spectral grid is sufficient to derive WR stellar parameters quickly and could provide more accurate initial parameter input to the PoWR program code.

关 键 词：stars:massive stars:mass-loss stars:Wolf-Rayet stars:atmospheres stars:winds OUTFLOWS 

分 类 号：P152[天文地球—天文学]