Abstract
Spectroscopic and photometric variations of the central star of the planetary nebula PRTM 1 (PN G243.8-37.1) have been detected from optical spectrophotometric data. The photometric variations can be as large as ΔV~1 mag, but most of the time they are within 0.2 mag. The phenomenon seems to be cyclic. These optical changes confirm the UV variations reported by W. Feibelman from IUE archived data. The star presents a highly ionized spectrum, showing absorption lines of H I and He II. The stellar features also change, becoming deeper when the star is brighter, while at the same time the C IV λ5808 doublet appears in emission. The star cannot be classified as an "O VI" star, as proposed by W. Feibelman, because the optical O VI lines are absent from the spectrum. The nebular lines show no sign of variation. The possible origin of the stellar changes is discussed.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
