Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71
<i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massi...
Ausführliche Beschreibung
Autor*in: |
Mehner, Andrea - 1981- [verfasserIn] Stahl, Otmar [verfasserIn] |
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Format: |
E-Artikel |
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Sprache: |
Englisch |
Erschienen: |
15 December 2017 |
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Anmerkung: |
Gesehen am 24.09.2018 |
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Umfang: |
18 |
Übergeordnetes Werk: |
Enthalten in: Astronomy and astrophysics - Les Ulis : EDP Sciences, 1969, 608(2017) Artikel-Nummer A124, 18 Seiten |
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Übergeordnetes Werk: |
volume:608 ; year:2017 ; extent:18 |
Links: |
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DOI / URN: |
10.1051/0004-6361/201731829 |
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Katalog-ID: |
1581222130 |
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245 | 1 | 0 | |a Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 |c A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl |
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520 | |a <i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. | ||
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10.1051/0004-6361/201731829 doi (DE-627)1581222130 (DE-576)511222130 (DE-599)BSZ511222130 (OCoLC)1341018943 DE-627 ger DE-627 rda eng Mehner, Andrea 1981- verfasserin (DE-588)1167705416 (DE-627)1031227954 (DE-576)511221673 aut Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl 15 December 2017 18 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 24.09.2018 <i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Stahl, Otmar verfasserin (DE-588)1035490730 (DE-627)747597537 (DE-576)163157715 aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 608(2017) Artikel-Nummer A124, 18 Seiten Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:608 year:2017 extent:18 http://dx.doi.org/10.1051/0004-6361/201731829 Verlag Resolving-System kostenfrei Volltext https://www.aanda.org/articles/aa/pdf/2017/12/aa31829-17.pdf Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2021 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 608 2017 18 608(2017) Artikel-Nummer A124, 18 Seiten 2013 01 DE-16-250 3026234648 00 --%%-- --%%-- --%%-- --%%-- l01 24-09-18 2403 01 DE-LFER 3028301350 00 --%%-- --%%-- n --%%-- l01 10-10-18 2403 01 DE-LFER http://dx.doi.org/10.1051/0004-6361/201731829 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_10 2013 01 DE-16-250 03 s s_18 2013 01 DE-16-250 04 p (DE-627)1453059474 Stahl, Otmar 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_10 |
spelling |
10.1051/0004-6361/201731829 doi (DE-627)1581222130 (DE-576)511222130 (DE-599)BSZ511222130 (OCoLC)1341018943 DE-627 ger DE-627 rda eng Mehner, Andrea 1981- verfasserin (DE-588)1167705416 (DE-627)1031227954 (DE-576)511221673 aut Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl 15 December 2017 18 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 24.09.2018 <i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Stahl, Otmar verfasserin (DE-588)1035490730 (DE-627)747597537 (DE-576)163157715 aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 608(2017) Artikel-Nummer A124, 18 Seiten Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:608 year:2017 extent:18 http://dx.doi.org/10.1051/0004-6361/201731829 Verlag Resolving-System kostenfrei Volltext https://www.aanda.org/articles/aa/pdf/2017/12/aa31829-17.pdf Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2021 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 608 2017 18 608(2017) Artikel-Nummer A124, 18 Seiten 2013 01 DE-16-250 3026234648 00 --%%-- --%%-- --%%-- --%%-- l01 24-09-18 2403 01 DE-LFER 3028301350 00 --%%-- --%%-- n --%%-- l01 10-10-18 2403 01 DE-LFER http://dx.doi.org/10.1051/0004-6361/201731829 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_10 2013 01 DE-16-250 03 s s_18 2013 01 DE-16-250 04 p (DE-627)1453059474 Stahl, Otmar 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_10 |
allfields_unstemmed |
10.1051/0004-6361/201731829 doi (DE-627)1581222130 (DE-576)511222130 (DE-599)BSZ511222130 (OCoLC)1341018943 DE-627 ger DE-627 rda eng Mehner, Andrea 1981- verfasserin (DE-588)1167705416 (DE-627)1031227954 (DE-576)511221673 aut Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl 15 December 2017 18 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 24.09.2018 <i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Stahl, Otmar verfasserin (DE-588)1035490730 (DE-627)747597537 (DE-576)163157715 aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 608(2017) Artikel-Nummer A124, 18 Seiten Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:608 year:2017 extent:18 http://dx.doi.org/10.1051/0004-6361/201731829 Verlag Resolving-System kostenfrei Volltext https://www.aanda.org/articles/aa/pdf/2017/12/aa31829-17.pdf Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2021 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 608 2017 18 608(2017) Artikel-Nummer A124, 18 Seiten 2013 01 DE-16-250 3026234648 00 --%%-- --%%-- --%%-- --%%-- l01 24-09-18 2403 01 DE-LFER 3028301350 00 --%%-- --%%-- n --%%-- l01 10-10-18 2403 01 DE-LFER http://dx.doi.org/10.1051/0004-6361/201731829 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_10 2013 01 DE-16-250 03 s s_18 2013 01 DE-16-250 04 p (DE-627)1453059474 Stahl, Otmar 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_10 |
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10.1051/0004-6361/201731829 doi (DE-627)1581222130 (DE-576)511222130 (DE-599)BSZ511222130 (OCoLC)1341018943 DE-627 ger DE-627 rda eng Mehner, Andrea 1981- verfasserin (DE-588)1167705416 (DE-627)1031227954 (DE-576)511221673 aut Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl 15 December 2017 18 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 24.09.2018 <i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Stahl, Otmar verfasserin (DE-588)1035490730 (DE-627)747597537 (DE-576)163157715 aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 608(2017) Artikel-Nummer A124, 18 Seiten Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:608 year:2017 extent:18 http://dx.doi.org/10.1051/0004-6361/201731829 Verlag Resolving-System kostenfrei Volltext https://www.aanda.org/articles/aa/pdf/2017/12/aa31829-17.pdf Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2021 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 608 2017 18 608(2017) Artikel-Nummer A124, 18 Seiten 2013 01 DE-16-250 3026234648 00 --%%-- --%%-- --%%-- --%%-- l01 24-09-18 2403 01 DE-LFER 3028301350 00 --%%-- --%%-- n --%%-- l01 10-10-18 2403 01 DE-LFER http://dx.doi.org/10.1051/0004-6361/201731829 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_10 2013 01 DE-16-250 03 s s_18 2013 01 DE-16-250 04 p (DE-627)1453059474 Stahl, Otmar 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_10 |
allfieldsSound |
10.1051/0004-6361/201731829 doi (DE-627)1581222130 (DE-576)511222130 (DE-599)BSZ511222130 (OCoLC)1341018943 DE-627 ger DE-627 rda eng Mehner, Andrea 1981- verfasserin (DE-588)1167705416 (DE-627)1031227954 (DE-576)511221673 aut Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl 15 December 2017 18 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 24.09.2018 <i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Stahl, Otmar verfasserin (DE-588)1035490730 (DE-627)747597537 (DE-576)163157715 aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 608(2017) Artikel-Nummer A124, 18 Seiten Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:608 year:2017 extent:18 http://dx.doi.org/10.1051/0004-6361/201731829 Verlag Resolving-System kostenfrei Volltext https://www.aanda.org/articles/aa/pdf/2017/12/aa31829-17.pdf Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2021 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 608 2017 18 608(2017) Artikel-Nummer A124, 18 Seiten 2013 01 DE-16-250 3026234648 00 --%%-- --%%-- --%%-- --%%-- l01 24-09-18 2403 01 DE-LFER 3028301350 00 --%%-- --%%-- n --%%-- l01 10-10-18 2403 01 DE-LFER http://dx.doi.org/10.1051/0004-6361/201731829 2013 01 DE-16-250 00 s hd2017 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_10 2013 01 DE-16-250 03 s s_18 2013 01 DE-16-250 04 p (DE-627)1453059474 Stahl, Otmar 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_10 |
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Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 |
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Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl |
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spectroscopic and photometric oscillatory envelope variability during the s doradus outburst of the luminous blue variable r71 |
title_auth |
Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 |
abstract |
<i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Gesehen am 24.09.2018 |
abstractGer |
<i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Gesehen am 24.09.2018 |
abstract_unstemmed |
<i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. As in the case of RV Tau variables, the occurrence of double absorption lines with an apparent regular cycle may be due to shocks within the atmosphere and period doubling may explain the factor of two in the lengths of the photometric and spectroscopic cycles. Gesehen am 24.09.2018 |
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Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71 |
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http://dx.doi.org/10.1051/0004-6361/201731829 https://www.aanda.org/articles/aa/pdf/2017/12/aa31829-17.pdf |
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Mehner, A. Mehner, Andrea Stahl, Otto Stahl, Otmar |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a2200265 4500</leader><controlfield tag="001">1581222130</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220815015250.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180924s2017 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1051/0004-6361/201731829</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)1581222130</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-576)511222130</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)BSZ511222130</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(OCoLC)1341018943</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rda</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Mehner, Andrea</subfield><subfield code="d">1981-</subfield><subfield code="e">verfasserin</subfield><subfield code="0">(DE-588)1167705416</subfield><subfield code="0">(DE-627)1031227954</subfield><subfield code="0">(DE-576)511221673</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71</subfield><subfield code="c">A. Mehner, D. Baade, J. H. Groh, T. Rivinius, F.-J. Hambsch, E. S. Bartlett, D. Asmus, C. Agliozzo, T. Szeifert, and O. Stahl</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">15 December 2017</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">18</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">Gesehen am 24.09.2018</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a"><i>Context. <i/>Luminous blue variables (LBVs) are evolved massive stars that exhibit instabilities that are not yet understood. Stars can lose several solar masses during this evolutionary phase. The LBV phenomenon is thus critical to our understanding of the evolution of the most massive stars.<i>Aims. <i/>The LBV R71 in the Large Magellanic Cloud is presently undergoing an S Doradus outburst, which started in 2005. To better understand the LBV phenomenon, we determine the fundamental stellar parameters of R71 during its quiescence phase. In addition, we analyze multiwavelength spectra and photometry obtained during the current outburst.<i>Methods. <i/>We analyzed pre-outburst CASPEC spectra from 1984-1997, EMMI spectra in 2000, UVES spectra in 2002, and FEROS spectra from 2005 with the radiative transfer code CMFGEN to determine the fundamental stellar parameters of the star. A spectroscopic monitoring program with VLT X-shooter since 2012 secured visual to near-infrared spectra throughout the current outburst, which is well-covered by ASAS and AAVSO photometry. Mid-infrared images and radio data were also obtained.<i>Results. <i/>During quiescence, R71 has an effective temperature of <i>T<i/><sub>eff<sub/> = 15 500 K and a luminosity of log(<i>L<i/><sub>∗<sub/>/<i>L<i/><sub>⊙<sub/>) = 5.78. We determine its mass-loss rate to 4.0 × 10<sup>-6<sup/><i>M<i/><sub>⊙<sub/> yr<sup>-1<sup/>. We present the spectral energy distribution of R71 from the near-ultraviolet to the mid-infrared during its present outburst. Semi-regular oscillatory variability in the light curve of the star is observed during the current outburst. Absorption lines develop a second blue component on a timescale of twice that length. The variability may consist of one (quasi-)periodic component with <i>P<i/> ~ 425/850 d with additional variations superimposed.<i>Conclusions. <i/>R71 is a classical LBV, but this star is at the lower luminosity end of this group. Mid-infrared observations suggest that we are witnessing dust formation and grain evolution. During its current S Doradus outburst, R71 occupies a region in the HR diagram at the high-luminosity extension of the Cepheid instability strip and exhibits similar irregular variations as RV Tau variables. LBVs do not pass the Cepheid instability strip because of core evolution, but they develop comparable cool, low-mass, extended atmospheres in which convective instabilities may occur. 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