magnetic fields in intermediate mass t-tauri stars › uusu2014 › pdf › ... · proto-star...
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Magnetic fields in Intermediate Mass T-Tauri Stars
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #1/21
Alexis LavailUppsala Universitet
Supervisors: Oleg Kochukhov & Nikolai Piskunov
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→ Stellar magnetic fieldscool stars against hot stars
For cool stars such as the Sun,the magnetic field is:
> rapidly evolving> complex> weak
Hot stars tend to present magnetic fields which are:
> very strong> organized> roughly dipolar
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #2/21
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→ Stellar magnetic fieldscool stars against hot stars
For cool stars such as the Sun,the magnetic field is:
> rapidly evolving> complex> weak
Hot stars tend to present magnetic fields which are:
> very strong> organized> roughly dipolar
““FOSSIL” FIELDFOSSIL” FIELDDYNAMO-GENERATED FIELDDYNAMO-GENERATED FIELD
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #3/21
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→ Stellar magnetic fieldsdynamo against fossil fields
DYNAMO-GENERATED FIELD ““FOSSIL” FIELDFOSSIL” FIELDDYNAMO-GENERATED FIELDDYNAMO-GENERATED FIELD
Uncertain origin of fossil field ..
> galactic magnetic field captured by the star ?> leftovers from dynamo processes ?
?
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #4/21
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→ Intermediate Mass T-Tauri stars (IMTTS)in stellar evolution context
proto-star T-Tauri star Main-Sequence star
Pre-Main Sequence (PMS) Main Sequence (MS)
T-Tauri stars:> roughly between 0.5 and 3.5 solar masses> accreting material from surrounding protoplanetary disc> fueled by gravitational energy from star's contraction
Intermediate Mass T-Tauri Stars:> around 2 solar masses> progenitors of Herbig Ae/Be stars and ultimately A/B type stars
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #5/21
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→ Intermediate Mass T-Tauri stars (IMTTS)in stellar evolution context
HR diagram from Evelyne Alecian http://astars2013.inasan.ru/presentations/4_06/Alecian/Alecian_Moscou.pdf
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #6/21
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→ Intermediate Mass T-Tauri stars (IMTTS)in stellar evolution context
HR diagram from Evelyne Alecian http://astars2013.inasan.ru/presentations/4_06/Alecian/Alecian_Moscou.pdf
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #7/21
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→ Intermediate Mass T-Tauri stars (IMTTS)in stellar evolution context
HR diagram from Evelyne Alecian http://astars2013.inasan.ru/presentations/4_06/Alecian/Alecian_Moscou.pdf
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #8/21
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→ Intermediate Mass T-Tauri stars (IMTTS)in stellar evolution context
HR diagram from Evelyne Alecian http://astars2013.inasan.ru/presentations/4_06/Alecian/Alecian_Moscou.pdf
IMTTS
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #9/21
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→ Intermediate Mass T-Tauri stars (IMTTS)and their magnetic field
IMTTS Herbig Ae/Be Ap/Bp star
5-10 % host strong large-scale magneticfields
~10 % host strong large-scale magneticfields
Low-Mass T-Tauri Stars
complex magnetic fields generated by dynamo processes
both large scale and complex magnetic fields
Science case:Studying evolution of magnetic field with the age of IMTTS to see if: → fields goes from “dynamo” to “fossil” → dynamo fields gradually disappear while
fossil fields stay in constant proportion
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #10/21
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→ Observing stellar magnetic fieldZeeman effect in stellar spectra
Zeeman effectFirst observed by Zeeman in 1896
First observable> Spectral lines split into several components when a magnetic field is present
>> the component shift is proportional to the magnetic field strength, wavelength, and Landé factor
Δλ = 0.00467 g λ² |B| Δλ is the component shift in nmλ is the wavelength in μ mg is the Landé factor of the component B is the m.f. strength in kG
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #11/21
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→ Observing stellar magnetic fieldZeeman effect in stellar spectra
Second observable> The π and σ components exhibit linear or/and circular polarization according to the magnetic field orientation w.r.t. the line of sight.
Image from "Observations of Cool-Star Magnetic Fields" by Ansgar Reinershttp://solarphysics.livingreviews.org/Articles/lrsp-2012-1/
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #12/21
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→ Detection methodspectral synthesis with no magnetic field
Atomic data
Model atmosphere
Vienna Atomic Line DatabaseVALD
MARCS
Wavelengths, Landé factors, oscillator strengths, energy levels etc …
Effective temperature & surface gravity
Spectral synthesis code
SYNMAST
No magnetic field
synthetic spectrum
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #13/21
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→ Detection methodComparison between synthetic and observed spectra
Atomic data
Model atmosphere
Vienna Atomic Line DatabaseVALD
MARCS
Wavelengths, Landé factors, oscillator strengths, energy levels etc …
Effective temperature & surface gravity
Spectral synthesis code
SYNMAST
synthetic spectrum
observed spectrum
Comparison
No magnetic field
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #14/21
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→ Detection methodspectral synthesis with magnetic field
synthetic spectrum
observed spectrum
ComparisonUse of weakly sensitive and non sensitive to constrain non-magnetic broadening
SYNMAST
strength of the magnetic field
SYNMAST
Spectral synthesis code
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #15/21
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Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #16/21
→ Improving atomic datawith the Sun as a benchmark H-band
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Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #17/21
→ Improving atomic datawith the Sun as a benchmark H-band
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Our spectra are acquired:
→ with the CRIRES instrument sitting at the VLT
→ for ~10 stars with effective temperature roughly between 4000 K and 6000 K
→ in 2 infrared spectral bands: H-band (around 1.56 µm) and K-band (around 2.31 µm)
Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #18/21
H-band K-band
→ ObservationsSpectra in H and K band
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Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #19/21
→ Real dataylw19 H-band
no magnetic field
2 kG radial magnetic field
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Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #20/21
→ Future workNow what?
→ Work on all the spectra and try to get upper limit on magnetic field strength
→ Involvement in the upgrade of the CRIRES instrument
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Alexis Lavail – SU/UU PhD days @Uppsala - 2014.04.10 – #21/21
Thanks for listening