observing the brightest stars - files.warwick · 2017. 9. 12. · the brightest stars provide the...
TRANSCRIPT
-
Observing the brightest stars
Tim WhiteStellar Astrophysics Centre, Aarhus University
-
Why bright stars?
205/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
305/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
405/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
505/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
We need to use all of the tools at our disposal:
605/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
We need to use all of the tools at our disposal:• Asteroseismology
705/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
We need to use all of the tools at our disposal:• Asteroseismology
• Spectroscopy
805/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
We need to use all of the tools at our disposal:• Asteroseismology
• Spectroscopy
• Interferometry
905/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
We need to use all of the tools at our disposal:• Asteroseismology
• Spectroscopy
• Interferometry
• Polarimetry
1005/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why bright stars?
We want to characterize stars with the greatest possible precision:
• In order to provide the most stringent tests of stellar models
• In order to achieve the best possible characterization of exoplanets
We need to use all of the tools at our disposal:• Asteroseismology
• Spectroscopy
• Interferometry
• Polarimetry
A long history of observations.1105/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 12
-
Why not bright stars?
1305/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why not bright stars?
SaturationOften our instruments are built to observe many faint stars.
1405/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why not bright stars?
SaturationOften our instruments are built to observe many faint stars.
1505/09/2017 PLATO Mission Conference 2017 – University of Warwick
-
Why not bright stars?
SaturationOften our instruments are built to observe many faint stars.
1605/09/2017 PLATO Mission Conference 2017 – University of Warwick
Arkūshanangarushash
ūtu
-
Why not bright stars?
SaturationOften our instruments are built to observe many faint stars.
Sometimes their names are hard to pronounce
1705/09/2017 PLATO Mission Conference 2017 – University of Warwick
Arkūshanangarushash
ūtu
-
Overcoming saturation
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 18
-
Overcoming saturation
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 19
-
Overcoming saturation
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 20
-
Overcoming saturation
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 21
-
Overcoming saturation
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 22
-
HD 185351 – a ‘retired’ A star?
Problem: It’s difficult to conduct RV surveys around A-type stars. How can we find out about the population of planets aroundintermediate-mass stars?
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 23
-
HD 185351 – a ‘retired’ A star?
Problem: It’s difficult to conduct RV surveys around A-type stars. How can we find out about the population of planets aroundintermediate-mass stars?
Solution: Wait until they evolve into cooler subgiants and giants.
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 24
-
HD 185351 – a ‘retired’ A star?
Problem: It’s difficult to conduct RV surveys around A-type stars. How can we find out about the population of planets aroundintermediate-mass stars?
Solution: Wait until they evolve into cooler subgiants and giants.
Problem: How can you be sure these stars are evolved A stars?
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 25
-
HD 185351 – a ‘retired’ A star?
Problem: It’s difficult to conduct RV surveys around A-type stars. How can we find out about the population of planets around intermediate-mass stars?
Solution: Wait until they evolve into cooler subgiants and giants.
Problem: How can you be sure these stars are evolved A stars?Solution: Characterize them with asteroseismology and
complementary techniques.
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 26
-
HD 185351 – a ‘retired’ A star?
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 27
Johnson et al. 2014, ApJ 794, 15
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 28
HD 185351 – a ‘retired’ A star?
Hjørringgaard et al. 2017, MNRAS 464, 3713
1.5 Mʘ2.0 Mʘ
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 29
Varying mixing length
1.5 Mʘ2.0 Mʘ1.5 Mʘ2.0 Mʘ
Hjørringgaard et al. 2017, MNRAS 464, 3713
αMLT= 2.00αMLT= 1.791
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 30
Including convective coreovershooting
1.5 Mʘ2.0 Mʘ 1.5 Mʘ
2.0 Mʘ
Hjørringgaard et al. 2017, MNRAS 464, 3713
αMLT= 2.00, f = 0.030αMLT= 1.791, f = 0
-
The Pleiades
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 31
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 32
-
‘Halo’ photometry
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 33
White et al. 2017, MNRAS 471, 2882
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 34
White et al. 2017, MNRAS 471, 2882
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 35
White et al. 2017, MNRAS 471, 2882
-
‘Halo’ photometry
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 36
𝑓𝑖 =
𝑗=1
𝑀
𝑤𝑗𝑝𝑖𝑗
https://github.com/hvidy/halophot
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 37
White et al. 2017, MNRAS 471, 2882
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 38
White et al. 2017, MNRAS 471, 2882
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 39
Figure courtesy of JCD
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 40
HypotheticalMaia Sequence
MAIA (4h?)
Figure courtesy of JCD Struve 1955, Sky & Telescope 14, 461
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 41
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 42
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 43
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 44
-
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 45
R = 6.61 ± 0.11 Rʘ
i = 90 °
v sin i = 33 ± 5 km s-1
T = 10.34 ± 0.09 d
+0
−30
-
Summary
The brightest stars provide the best opportunities to characterize stars and test stellar models.
We have learnt from previous missions how to overcome the problems caused by saturation to achieve high precision photometry. We will apply these lessons to observe the brightest stars with PLATO.
05/09/2017 PLATO Mission Conference 2017 – University of Warwick 46