Mass Transfer in Two Post-AGB Binaries with Dusty Disks
We present a time series of high-resolution spectra for two poorly studied candidate post-AGB stars surrounded by dusty disks, BD+46 442 and IRAS 19135+3937. We find that both stars show radial velocity variations with periods of 130-140 days. IRAS 19135+3937 has been previously classified as a semi...
| Main Authors: | , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
De Gruyter
2012-06-01
|
| Series: | Open Astronomy |
| Subjects: | |
| Online Access: | https://doi.org/10.1515/astro-2017-0371 |
| _version_ | 1818366494077091840 |
|---|---|
| author | Gorlova N. Van Winckel H. Jorissen A. |
| author_facet | Gorlova N. Van Winckel H. Jorissen A. |
| author_sort | Gorlova N. |
| collection | DOAJ |
| description | We present a time series of high-resolution spectra for two poorly studied candidate post-AGB stars surrounded by dusty disks, BD+46 442 and IRAS 19135+3937. We find that both stars show radial velocity variations with periods of 130-140 days. IRAS 19135+3937 has been previously classified as a semi-regular variable based on the light variations with a similar period, but our spectra reveal an evolved star which is too warm to be on the AGB. the variability of BD+46 442 has not been studied till now. the stars reveal a number of spectroscopic peculiarities that resemble features in the interactive binaries including the S-type Symbiotics. Namely, H profile alternates between a double-peak emission and a P Cyg profile, which correlates with the radial velocity phase. A weak asymmetry is tentatively detected in the cross-correlation function that moves in anti-phase with the main component. In addition, strong photospheric lines reveal a narrow central absorption. We conclude that these peculiarities are consistent with a picture where the observed post-AGB stars orbit a much fainter companion at a sub-AU separation and transfer mass on it. the companion is surrounded by an accretion disk, possibly with some kind of an outflow. the SED shows that whole system is surrounded by stable dusty disk as well. It remains to be seen with more observations how much of the line asymmetry could be due to the contribution of low-amplitude pulsations. |
| first_indexed | 2024-12-13T22:37:03Z |
| format | Article |
| id | doaj.art-de6f4689ea3b465b89ff769554f31200 |
| institution | Directory Open Access Journal |
| issn | 2543-6376 |
| language | English |
| last_indexed | 2024-12-13T22:37:03Z |
| publishDate | 2012-06-01 |
| publisher | De Gruyter |
| record_format | Article |
| series | Open Astronomy |
| spelling | doaj.art-de6f4689ea3b465b89ff769554f312002022-12-21T23:28:57ZengDe GruyterOpen Astronomy2543-63762012-06-01211-216517110.1515/astro-2017-0371astro-2017-0371Mass Transfer in Two Post-AGB Binaries with Dusty DisksGorlova N.0Van Winckel H.1Jorissen A.2Institute of Astronomy, Catholic University of Leuven, Celestijnenlaan 200D, Bus 2401, Leuven, BelgiumInstitute of Astronomy, Catholic University of Leuven, Celestijnenlaan 200D, Bus 2401, Leuven, BelgiumInstitute of Astronomy and Astrophysics, Free University of Brussels, CP 226, Boulevard du Triomphe, 1050, Brussels, BelgiumWe present a time series of high-resolution spectra for two poorly studied candidate post-AGB stars surrounded by dusty disks, BD+46 442 and IRAS 19135+3937. We find that both stars show radial velocity variations with periods of 130-140 days. IRAS 19135+3937 has been previously classified as a semi-regular variable based on the light variations with a similar period, but our spectra reveal an evolved star which is too warm to be on the AGB. the variability of BD+46 442 has not been studied till now. the stars reveal a number of spectroscopic peculiarities that resemble features in the interactive binaries including the S-type Symbiotics. Namely, H profile alternates between a double-peak emission and a P Cyg profile, which correlates with the radial velocity phase. A weak asymmetry is tentatively detected in the cross-correlation function that moves in anti-phase with the main component. In addition, strong photospheric lines reveal a narrow central absorption. We conclude that these peculiarities are consistent with a picture where the observed post-AGB stars orbit a much fainter companion at a sub-AU separation and transfer mass on it. the companion is surrounded by an accretion disk, possibly with some kind of an outflow. the SED shows that whole system is surrounded by stable dusty disk as well. It remains to be seen with more observations how much of the line asymmetry could be due to the contribution of low-amplitude pulsations.https://doi.org/10.1515/astro-2017-0371starsagb and post-agbbinariesspectroscopic |
| spellingShingle | Gorlova N. Van Winckel H. Jorissen A. Mass Transfer in Two Post-AGB Binaries with Dusty Disks Open Astronomy stars agb and post-agb binaries spectroscopic |
| title | Mass Transfer in Two Post-AGB Binaries with Dusty Disks |
| title_full | Mass Transfer in Two Post-AGB Binaries with Dusty Disks |
| title_fullStr | Mass Transfer in Two Post-AGB Binaries with Dusty Disks |
| title_full_unstemmed | Mass Transfer in Two Post-AGB Binaries with Dusty Disks |
| title_short | Mass Transfer in Two Post-AGB Binaries with Dusty Disks |
| title_sort | mass transfer in two post agb binaries with dusty disks |
| topic | stars agb and post-agb binaries spectroscopic |
| url | https://doi.org/10.1515/astro-2017-0371 |
| work_keys_str_mv | AT gorlovan masstransferintwopostagbbinarieswithdustydisks AT vanwinckelh masstransferintwopostagbbinarieswithdustydisks AT jorissena masstransferintwopostagbbinarieswithdustydisks |