2014A&A...567A..15H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST03:16:32

2014A&A...567A..15H - Astronomy and Astrophysics, volume 567A, 15-15 (2014/7-1)

The evolving spectrum of the planetary nebula Hen 2-260.

HAJDUK M., VAN HOOF P.A.M., GESICKI K., ZIJLSTRA A.A., GORNY S.K. and GLADKOWSKI M.

Abstract (from CDS):

We analysed the planetary nebula Hen2-260 using optical spectroscopy and photometry. We compared our observations with the data from literature to search for evolutionary changes. We also searched for photomertic variability of the central star. The object Hen2-260 was observed with the SAAO 1.0m telescope (photometry) and the SALT telescope (low resolution spectroscopy). We also used archival high resolution Very Large Telescope spectra and Hubble Space Telescope imaging. The nebular line fluxes were modelled with the Cloudy photoionization code to derive the stellar and nebular parameters. The planetary nebula shows a complex structure and possibly a bipolar outflow. The nebula is relatively dense and young. The central star is just starting O+ ionization (Teff≃30000K). Comparison of our observations with literature data indicates a 50% increase of the [OIII] 5007Å line flux between 2001 and 2012. We interpret it as the result of the progression of the ionization of O+. The central star evolves to higher temperatures at a rate of 45±7K/yr. The heating rate is consistent with a final mass of 0.626+0.003–0.005M or 0.645+0.008–0.008M for two different sets of post-AGB evolutionary tracks from literature. The photometric monitoring of Hen2-260 revealed variations on a timescale of hours or days. There is no direct indication for central star binarity in the spectrum nor for a strong stellar wind. The variability may be caused by pulsations of the star. The temperature evolution of the central star can be traced using spectroscopic observations of the surrounding planetary nebula spanning a timescale of roughly a decade. This allows us to precisely determine the stellar mass, since the pace of the temperature evolution depends critically on the core mass. The method is independent of the absolute age of the nebula. The kinematical age of the nebula is consistent with the age obtained from the evolutionary track. The final mass of the central star is close to the mass distribution peak for central stars of planetary nebulae found in other studies. The object belongs to a group of young central stars of planetary nebulae showing photometric variability.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - stars: evolution - planetary nebulae: general - planetary nebulae: individual: Hen 2-260

VizieR on-line data: <Available at CDS (J/A+A/567/A15): table4.dat>

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 CD-59 6479 Be* 17 16 21.08 -59 29 23.3 10.03 10.73 10.75     B3e 112 0
2 PN SaSt 2-15 PN 17 38 57.3716181503 -18 17 35.779247942   13.93 13.66 13.82   ~ 69 0
3 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11540 0
4 NGC 6572 PN 18 12 06.3140077888 +06 51 13.030152295   9.3 10.8     [WC] 738 0
5 IC 4997 PN 20 20 08.7615653034 +16 43 53.993812400   11.94 11.15     [WC7/8] 528 0
6 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2323 1

    Equat.    Gal    SGal    Ecl

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2020.07.10-03:16:32

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