Please use this identifier to cite or link to this item:
Title: SAO 244567 - A post-AGB star which has turned into a planetary nebula within the last 40 years
Authors: Parthasarathy, M
Garcia-Lario, P
Pottasch, S. R
Manchando, A
Clavel, J
de Martino, D
Van de Steene, G. C. M
Sahu, K. C
Keywords: Asymptotic giant branch stars;Infrared astronomy satellite;Planetary nebulae;Stellar mass ejection;Early stars;Infrared stars;Ultraviolet radiation
Issue Date: Jan-1993
Publisher: European Sothern Observatory
Citation: Astronomy and Astrophysics , Vol. 267, No. 1, pp. L19 - L22
Abstract: SAO 244567 (Hen 1357 = CPD -59 deg 6926 = IRAS 17119-5926) is an IRAS source with far infrared colors and flux distribution similar to those of planetary nebulae. The IUE ultraviolet spectra obtained in July 1988 and April 1992 show nebular emission lines, and also the changes in the spectra suggest the formation of the planetary nebula and the rapid evolution of the central star. The optical spectrum of this star obtained by Henize around 1950 shows only the H-alpha line in emission, while the most recent one, obtained in 1990 shows strong forbidden emission lines corresponding to a low excitation and young planetary nebula. The IUE ultraviolet spectra show evidence for the presence of stellar wind and mass loss. The stellar lines show P-Cygni type profiles and the terminal velocity of the stellar wind is about - 3000 km/s. The spectral type of the central star is O8 V. The presence of a detached cold dust shell (125 K), high galactic latitude and abundances suggest that SAO 244567 has recently evolved from a low or intermediate mass progenitor star which has ejected its outer envelope during the AGB stage of evolution and is rapidly evolving towards hotter spectral types.
ISSN: 0004-6361
Appears in Collections:IIAP Publications

Files in This Item:
File Description SizeFormat 
Partha1.pdf758.1 kBAdobe PDFView/Open

Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.