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The compact H$\alpha$ emitting regions of the Herbig Ae/Be stars HD 179218 and HD 141569 from CHARA spectro-interferometry
Solar and Stellar Astrophysics · Submitted 30 Sep 2016
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Putting the CHARA sample together, a variety of scenarios is required to explain the H$\alpha$ emission in HAeBe stars -compact or extended, discs, accretion, and winds-, in agreement with previous Br$\gamma$ spectro-interferometric observations.
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The abstract, sentence by sentence
This work presents CHARA/VEGA H$\alpha$ spectro-interferometry (R ~ 6000, and $\lambda$/2B ~ 1 mas) of HD 179218 and HD 141569, doubling the sample of Herbig Ae/Be (HAeBe) stars for which this type of observations is available so far. The observed H$\alpha$ emission is spatially unresolved, indicating that the size of the H$\alpha$ emitting region is smaller than ~ 0.21 and 0.12 au for HD 179218 and HD 141529 (~ 15 and 16 R*, respectively). This is smaller than for the two other HAeBes previously observed with the same instrumentation. Two different scenarios have been explored in order to explain the compact line emitting regions. A hot, several thousand K, blackbody disc is consistent with the observations of HD 179218 and HD 141569. Magnetospheric accretion (MA) is able to reproduce the bulk of the H$\alpha$ emission shown by HD 179218, confirming previous estimates from MA shock modelling with a mass accretion rate of 10^-8 Msun/yr, and an inclination to the line of sight between 30 and 50 degr. The H$\alpha$ profile of HD 141569 cannot be fitted from MA due to the high rotational velocity of this object. Putting the CHARA sample together, a variety of scenarios is required to explain the H$\alpha$ emission in HAeBe stars -compact or extended, discs, accretion, and winds-, in agreement with previous Br$\gamma$ spectro-interferometric observations.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | This work presents CHARA/VEGA H$\alpha$ spectro-interferometry (R ~ 6000, and $\lambda$/2B ~ 1 mas) of HD 179218 and HD 141569, doubling the sample of Herbig Ae/Be (HAeBe) stars for which this type of observations is available so far. | contribution 0.93 | 0.96 | 0.08 | asserted 1.00 |
| s1 | The observed H$\alpha$ emission is spatially unresolved, indicating that the size of the H$\alpha$ emitting region is smaller than ~ 0.21 and 0.12 au for HD 179218 and HD 141529 (~ 15 and 16 R*, respectively). | result 0.98 | 0.94 | 0.28 | hedged possibility 0.80 |
| s2 | This is smaller than for the two other HAeBes previously observed with the same instrumentation. | result 0.79 | 0.69 | 0.11 | asserted 1.00 |
| s3 | Two different scenarios have been explored in order to explain the compact line emitting regions. | method 0.38 | 0.70 | 0.05 | asserted 0.89 |
| s4 | A hot, several thousand K, blackbody disc is consistent with the observations of HD 179218 and HD 141569. | interpretation 0.95 | 0.79 | 0.14 | hedged possibility 0.98 |
| s5 | Magnetospheric accretion (MA) is able to reproduce the bulk of the H$\alpha$ emission shown by HD 179218, confirming previous estimates from MA shock modelling with a mass accretion rate of 10^-8 Msun/yr, and an inclination to the line of sight between 30 and 50 degr. | interpretation 0.62 | 0.73 | 0.12 | asserted 0.75 |
| s6 | The H$\alpha$ profile of HD 141569 cannot be fitted from MA due to the high rotational velocity of this object. | result 0.66 | 0.86 | 0.05 | asserted 1.00 |
| s7 | Putting the CHARA sample together, a variety of scenarios is required to explain the H$\alpha$ emission in HAeBe stars -compact or extended, discs, accretion, and winds-, in agreement with previous Br$\gamma$ spectro-interferometric observations. | interpretation 0.98 | 0.70 | 0.72 | asserted 0.95 |
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Original abstract
This work presents CHARA/VEGA H$\alpha$ spectro-interferometry (R ~ 6000, and $\lambda$/2B ~ 1 mas) of HD 179218 and HD 141569, doubling the sample of Herbig Ae/Be (HAeBe) stars for which this type of observations is available so far. The observed H$\alpha$ emission is spatially unresolved, indicating that the size of the H$\alpha$ emitting region is smaller than ~ 0.21 and 0.12 au for HD 179218 and HD 141529 (~ 15 and 16 R*, respectively). This is smaller than for the two other HAeBes previously observed with the same instrumentation. Two different scenarios have been explored in order to explain the compact line emitting regions. A hot, several thousand K, blackbody disc is consistent with the observations of HD 179218 and HD 141569. Magnetospheric accretion (MA) is able to reproduce the bulk of the H$\alpha$ emission shown by HD 179218, confirming previous estimates from MA shock modelling with a mass accretion rate of 10^-8 Msun/yr, and an inclination to the line of sight between 30 and 50 degr. The H$\alpha$ profile of HD 141569 cannot be fitted from MA due to the high rotational velocity of this object. Putting the CHARA sample together, a variety of scenarios is required to explain the H$\alpha$ emission in HAeBe stars -compact or extended, discs, accretion, and winds-, in agreement with previous Br$\gamma$ spectro-interferometric observations.
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