Volume 374, Number 1, July IV 2001
|Page(s)||L1 - L4|
|Published online||15 July 2001|
The companion of HD 190228: Planet or brown dwarf?*
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100012, PR China
2 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China
Corresponding author: G. Zhao, email@example.com
Accepted: 20 April 2001
A detailed abundance analysis has been carried out from high-resolution, high signal-to-noise spectra of the G5IV star HD 190228, which is announced to harbor an extrasolar planet with of 5.0 MJand an orbital period of 1127 days. Based on the model atmosphere of Teff=5180 K, , kms-1, we obtained , which puts it on the metal-poor tail of the metallicity distribution of the so far discovered 48 planet-harboring stars. The relative abundance, [X/Fe], indicates an overabundance of light elements (O, Na, Mg, Al, Si, S, Sc) by 0.1-0.2 dex and the solar abundance of heavier elements (K, Ca, Ti, V, Cr, Mn, Ni, Ba). These elements show no conspicuous anomalies. The solar [C/Fe] seems to be slightly smaller than the average (but within the scatter) of field stars of the same , and there is no clear trend of with condensation temperature of the element. Neither the process of planet formation nor the stellar dilution during the subgiant stage seems to have polluted its chemical composition. The initially low metallicity may be explained by the suggestion that HD 190228 is accompanied by a brown dwarf instead of a planet.
Key words: stars: abundances / planetary system
© ESO, 2001
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.