[vc_empty_space][vc_empty_space]
Spectral variations of the Be disk of δ-Scorpii during the 2011 periastron passage
Ahmad N.a, Zainuddin M.Z.a, Yahya M.S.a, Malasan H.L.b, Buil C.c
a Physics Department, Faculty of Science, University of Malaya, Kuala Lumpur, 50603, Malaysia
b Astronomy Division, FMIPA, Institut Teknologi Bandung, Bandung, 40132, Indonesia
c Astronomical Ring for Astronomy Spectroscopy, Castanet, 31400, France
[vc_row][vc_column][vc_row_inner][vc_column_inner][vc_separator css=”.vc_custom_1624529070653{padding-top: 30px !important;padding-bottom: 30px !important;}”][/vc_column_inner][/vc_row_inner][vc_row_inner layout=”boxed”][vc_column_inner width=”3/4″ css=”.vc_custom_1624695412187{border-right-width: 1px !important;border-right-color: #dddddd !important;border-right-style: solid !important;border-radius: 1px !important;}”][vc_empty_space][megatron_heading title=”Abstract” size=”size-sm” text_align=”text-left”][vc_column_text]© 2014 Elsevier B.V. All rights reserved.Mechanisms of the disk formation in Be stars may differ from one star to another and cause variations in the circumstellar disk’s spectral characters. δ-Scorpii is one of the bright Be binary stars that has been classified as a Be star since the 1990s when the star showed a weak Balmer emission line. In this work we study the characteristics of the Be disk of this star in the optical region during close encounters with its companion in order to investigate the appearance of the Be phenomenon. This work presents a monitoring and analysis of δ-Scorpii’s spectral character in the optical region during the 2011 periastron passage. The line profiles and strength (EW), relative intensity (I/Ic) and V/R ratio of the circumstellar regions Hα, Hβ, Hγ and HeI 6678 are used in the investigation of the Be disk characters of δ-Scorpii. We found that all physical characteristics of the line profiles such as equivalent width (EW), full width at half maximum (FWHM), etc. were enhanced during the time of the periastron. We suggest that the effects are owed to the tidal interaction of the companion in close encounters which might have a strong influence on the appearance and survival of the Be phenomenon of δ-Scorpii.[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Author keywords” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Indexed keywords” size=”size-sm” text_align=”text-left”][vc_column_text]Be star,Data analysis,Emission line profiles,Spectroscopy techniques[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Funding details” size=”size-sm” text_align=”text-left”][vc_column_text]IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”DOI” size=”size-sm” text_align=”text-left”][vc_column_text]https://doi.org/10.1016/j.newast.2014.10.002[/vc_column_text][/vc_column_inner][vc_column_inner width=”1/4″][vc_column_text]Widget Plumx[/vc_column_text][/vc_column_inner][/vc_row_inner][/vc_column][/vc_row][vc_row][vc_column][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][/vc_column][/vc_row]