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Exploring the magnetic activity of M dwarfs atnIR wavelengths with SPIRou
Julien MorinLaboratoire Univers et Particules de Montpellier
and the SPIRou Legacy Survey team
CFHT User’s meeting 2019 – Montréal – 20th May 2019
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Outline
1 M dwarfs’ magnetic activity and planet search
2 Magnetic activity of M dwarfs seen by SPIRou
3 Summary
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 2 / 15
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Outline
1 M dwarfs’ magnetic activity and planet searchImpact of stellar activity on planet detection and characterizationActive stars are everywhereActivity filteringGoing beyond the insolation HZStellar physics: : magnetism, activity, rotation
2 Magnetic activity of M dwarfs seen by SPIRou
3 Summary
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 3 / 15
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Impact of stellar activity on planet detection
� Activity effect on RV/photometricmeasurements
• Impede detection• Bias planetary parameters• False positives
Dittman et al. (2009)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 4 / 15
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Impact of stellar activity on planet detection
� Activity effect on RV/photometricmeasurements
• Impede detection• Bias planetary parameters• False positives
Dittman et al. (2009)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 4 / 15
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Impact of stellar activity on planet detection
� Activity effect on RV/photometricmeasurements
• Impede detection• Bias planetary parameters• False positives
Oshagh et al. (2013)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 4 / 15
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Impact of stellar activity on planet detection
� Activity effect on RV/photometricmeasurements
• Impede detection• Bias planetary parameters• False positives
Bonfils et al. (2007)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 4 / 15
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Impact of stellar activity on planet detection
� Activity effect on RV/photometricmeasurements
• Impede detection• Bias planetary parameters• False positives
Dumusque et al. (2011)SOAP model
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 4 / 15
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Active stars are everywhere
� Focus on low-mass stars• longer activity lifetimes• remain fast rotator longer• even slow rotators display activity� At high precision (almost) any star
is active
West et al. (2008)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 5 / 15
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Active stars are everywhere
� Focus on low-mass stars• longer activity lifetimes• remain fast rotator longer• even slow rotators display activity� At high precision (almost) any star
is active
Newton et al. (2016)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 5 / 15
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Active stars are everywhere
� Focus on low-mass stars• longer activity lifetimes• remain fast rotator longer• even slow rotators display activity� At high precision (almost) any star
is active
Bonfils et al. (2018)GJ 447 P ∼ 120 d
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 5 / 15
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Activity filtering: ZDI + DI
Donati et al. (2015, 2016)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 6 / 15
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Activity filtering: ZDI + DI
Donati et al. (2015, 2016)
Ô Louise Yu’s and Baptiste Klein’s talks
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 6 / 15
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Going beyond the insolation HZ
� Insolation HZ based on stellar flux� Role of magnetic field/activity
• XUV radiation• Stellar wind + magnetic pressure
å planetary magnetosphere balance� Need for evolutionary perspective
Credit: ESO/F. SelsisPR for Mayor et al. (2009)
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Going beyond the insolation HZ
� Insolation HZ based on stellar flux� Role of magnetic field/activity
• XUV radiation• Stellar wind + magnetic pressure
å planetary magnetosphere balance� Need for evolutionary perspective
France et al. (2018)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 7 / 15
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Going beyond the insolation HZ
� Insolation HZ based on stellar flux� Role of magnetic field/activity
• XUV radiation• Stellar wind + magnetic pressure
å planetary magnetosphere balance� Need for evolutionary perspective
Credit: NASA
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 7 / 15
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Going beyond the insolation HZ
� Insolation HZ based on stellar flux� Role of magnetic field/activity
• XUV radiation• Stellar wind + magnetic pressure
å planetary magnetosphere balance� Need for evolutionary perspective
Gallet & Bouvier (2015)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 7 / 15
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Going beyond the insolation HZ
� Insolation HZ based on stellar flux� Role of magnetic field/activity
• XUV radiation• Stellar wind + magnetic pressure
å planetary magnetosphere balance� Need for evolutionary perspective
Gallet et al. (2017)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 7 / 15
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Stellar physics: magnetism, activity, rotation
� Strong synergy w/ stellar science• stellar dynamos• magnetic cycles• angular momentum evolution
Ô large sampleÔ moderate-low activity regimeÔ baseline > 4 yr
Donati et al. (2008), Phan-Baoet al. (2009), Morin et al. (2008-2010),
Hébrard et al. (2016),Moutou et al. (2018)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 8 / 15
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Stellar physics: magnetism, activity, rotation
� Strong synergy w/ stellar science• stellar dynamos• magnetic cycles• angular momentum evolution
Ô large sampleÔ moderate-low activity regimeÔ baseline > 4 yr
Adapted from Reiners et al. (2009)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 8 / 15
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Outline
1 M dwarfs’ magnetic activity and planet search
2 Magnetic activity of M dwarfs seen by SPIRouMagnetometry: circular polarisationMagnetic activity: unpolarised spectra
3 Summary
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Magnetometry: circular polarisation
� Zeeman polarisation in spectral lines• Line-of-sight component of B• Cancellation Ô large-scalecomponent
• ∼ 1 000− 2 000 atomic lines
� V /Ic . few × 10−3
Ô Least-squares deconvolution (LSD)• ∼ 1 000− 2 000 atomic linesin the SPIRou spectral domain
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Toward LSD with molecular lines
� Molecules dominate M dwarfs’spectra
• line parameters poorly known• Landé factors not computable
Ô Experimental measurements• focus on H-band FeH, OH• detected in sunspots
Shulyak et al. (2010)FeH Wing-Ford band
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Toward LSD with molecular lines
� Molecules dominate M dwarfs’spectra
• line parameters poorly known• Landé factors not computable
Ô Experimental measurements• focus on H-band FeH, OH• detected in sunspots Credit: P. Crozet
experimental measurement
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 11 / 15
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Toward LSD with molecular lines
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Magnetic activity: unpolarised spectra
� Zeeman broadening/splitting• no cancellation effect• no information on vectorproperties
• ∆λB ∝ λ20
� For most active stars:• detect Zeeman splitting• multi-component models
� Chromospheric activity• HeI, Paβ, γ, δ• weaker emission wrt optical• K-band to be explored
Shöffer et al. (2019)
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Magnetic activity: unpolarised spectra
� Zeeman broadening/splitting• no cancellation effect• no information on vectorproperties
• ∆λB ∝ λ20
� For most active stars:• detect Zeeman splitting• multi-component models
� Chromospheric activity• HeI, Paβ, γ, δ• weaker emission wrt optical• K-band to be explored
Shöffer et al. (2019)
Julien Morin Magnetic activity of M dwarfs with SPIRou 20/05/2019 13 / 15
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Outline
1 M dwarfs’ magnetic activity and planet search
2 Magnetic activity of M dwarfs seen by SPIRou
3 Summary
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Summary
� Magnetic fields• Crucial for stellar physicsand for planetary systems
� Spectropolarimetry• ESPaDOnS legacy• SPIRou : ideal for M dwarfsmagnetism
� SLS• Huge potential for stellar science• Extended to very active / late SpT
Ô Build unique magnetic surveyÔ Include molecular lines in
spectropolarimetric analysis
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