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The central star of planetary nebula LT-5: A triple system
Malasan H.L.a,b,c, Yamasaki A.a,c,d,e, Kondo M.a,c
a Department of Astronomy, Faculty of Science, University of Tokyo, Japan
b Bosscha Observatory, Department of Astronomy, Bandung Institute of Technology, Indonesia
c Okayama Astrophysical Observatory, Dodaira Observatory, Natl. Astron. Observatory of Japan
d Mauna Kea Observatory, Institute of Astronomy, University of Hawaii
e Department of Geoscience, National Defense Academy, Japan
[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]Based upon photometric and spectroscopic studies, we confirm the previous suggestion by Jasniewicz et al. [A&A, 180, 145 (1987)] that IN Com, the central star of the planetary nebula LT-5, is a triple system. It is found from the present studies that the inner system consists of an evolved G-type star with active chromosphere and a low-mass companion, while the third body is a hot subdwarf exciting the surrounding planetary nebula. The light of the central star varies with a period of 1.20010 days though the levels of maximum and minimum light are not constant from cycle to cycle, and the phase of minimum light is changeable, due to photospheric and chromospheric disturbances on the surface of the G star. This period may be due to the rotation of the primary component. The spectral type is G5 III-IV. The present spectroscopic observations for radial velocities reveal that the inner system is a single-lined binary with period of 1.7545 days. The existence of a third body is deduced from the change of observed systemic velocities with a period of about 2000 days. The projected rotational velocity of the primary component is also determined to be 40 km/s. The orbital inclination of the inner system is found to be small (i < 24°). The primary's mass ranges from 0.7 to 1.9 ℳ⊙ and the secondary's mass is around 0.22ℳ⊙. The third body, a hot subdwarf, has a mass of around 1.1ℳ⊙. The distance, d = 100-170 pc, is in good agreement with that deduced from the statistical relation between distance and apparent diameter for large planetary nebulae.[/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][/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][/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/10.1086/115834[/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]