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 Hakim Luthfi Malasan;Bakuh Danang Setyo Budi

作者机构：Department of AstronomyFaculty of Mathematics and Natural SciencesInstitut Teknologi BandungBandung 40132Indonesia Bosscha ObservatoryInstitut Teknologi BandungLembang 40391Indonesia Master Program in AstronomyFaculty of Mathematics and Natural SciencesInstitut Teknologi BandungJl.Ganesha No.10Bandung 40132Indonesia 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2024年第24卷第9期

页      面：7-27页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

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 

主　　题：stars:massive stars:mass-loss stars:Wolf-Rayet stars:atmospheres stars:winds outflows 

摘      要：We present optical spectra of 10 Galactic Wolf-Rayet(WR)stars that consist of five WN and five WC *** 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,*** implemented stellar atmosphere Postdam Wolf-Rayet(PoWR)grid modeling to derive stellar *** normalized optical spectrum can be used to find the best model from the available PoWR grid,then we could derive stellar temperature and transformation *** 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 *** analysis to derive asymptotic terminal wind velocity was conducted from the P-Cygni profile analysis of the high-resolution IUE ultraviolet *** previously derived parameters,we could determine the mass loss rate of the WR ***,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.