asteroseismology,of,red,giants, observedbythe...
TRANSCRIPT
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Asteroseismology of red giants Observed by the Kepler Mission
Christina Hedges Mentors
Savita Mathur Keith MacGregor Michael Thompson
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Contents
• Introduction to Asteroseismology • Aims of Summer Project • Pipeline Creation • Results • Surface Rotation • Conclusions
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Red Giants
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Asteroseismology • What is Asteroseismology?
The study of oscillations in stars
Seismic activity in stars produces a Global Change in the stars surface, that is detectable.
• The oscillations in the stars have different modes. The oscillations are distinguished using l, m and n numbers.
• Low degree l modes are the easiest to identify as they produce a very obvious change to the star. l=0 modes are perceived as a breathing motion in the star.
• Two types of modes, p modes and g modes.
Image Credit: Birmingham Solar Oscillations Network. (BISON)
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Time/Flux data is converted to Frequency/Power data by Fourier Transform. This creates a Power Spectrum where modes appear as sharp peaks in a roughly Gaussian shaped group.
The spectrum is shaped and distorted by other factors from the star and satellite.
red giants due to their age and size have much lower frequency oscillations that solar like stars.
What do these Modes look like?
Frequency (microHz)
Power (p
pm)
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Modes are made up of thin Gaussian lines within a roughly Gaussian envelope. This structure is exhibited by all stars with oscillations. These modes are characterised mainly by two properties: • The Large Spacing: The space
between two modes of equal l number.
• The Frequency of Maximum Power: The frequency of the peak with the highest power.
These characteristics are linked to properties of the star.
Mean Large Frequency Spacing and Frequency of Maximum Power
Frequency (microHz)
Power (p
pm)
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• Using the KIC for effective temperature it is possible to utilise the mean large frequency spacing and the frequency of the maximum power to find Mass and Radius.
• The KIC is not perfect and has very large errors on effective temperature. This was corrected as much as possible using the findings from Thygesen et al. 2012
• Red giants have mixed g and p modes, making it possible to study the interiors of the stars.
What can Modes tell us?
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Aims • Automate this process so hundreds of red giants can
be easily analysed without the need for interaction. • Use these parameters to generate properties of the
stars. (Mass, Radius etc) • Use this data set to look into the surface rotation of
the red giant stars.
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Creating the Pipeline
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Example of Kepler Data
Image taken from star APH43664753 from Keplers Planet Hunters scheme
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• Each time series has between 1 and 2 years of data in it based on how long the exposure was from the Kepler satellite.
• The data was initially in units of e-‐/s and needed to be converted to ppm. This is done using the ppm KADACS routine. (Garcia et al. 2011)
• Infinite points where the satellite had problems such as saturation were converted to zeros.
• The LNP_TEST function was used to generate the power density spectrum.
Initial Data
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Two methods for background removal: • Fitting each individual
contribution of noise from each type of granulation and white noise contribution at high frequency
• Fitting the background with a fitting routine using a standard polynomial.
Background Removal
Frequency (microHz)
Power (p
pm)
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• After smoothing the Power Spectrum a sliding window is used to find the section with the highest power. (i.e. the envelope of modes.)
• The width is initially fixed but is later modified based on it’s position in the spectrum.
• The new window is used to find a value for νmax and the FWHM of the peak is taken to be the error.
Sliding Box
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• The power spectrum of the power spectrum shows any points that are periodic in frequency.
• As the modes are equally spaced in frequency there is a high power at the point that corresponds to this frequency. (Known as the mean large frequency spacing or Δν)
• Due to the l=1 mode this had to be doubled to correspond to the actual large spacing.
Second Power Spectrum
Frequency (microHz)
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*
Outliers and Corrections
Log(νmax)
Log(Δν
)
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The equations for Mass and Radius are given below.
These equations were taken from Mathur et al. 2010. Errors from Δν and νmax are propagated through.
Finding Radius and Mass
[Kjeldsen & Bedding 1995, Bedding & Kjeldsen 2003; Stello et al. 2008; Belkacen et al. 2011…]
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Comparison with KIC data
0
5
10
15
20
25
30
35
40
0 5 10 15 20 25 30 35 40
R from
KIC
R from Pipeline
Radius from KIC agains Radius from Pipeline
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0
5
10
15
20
25
30
35
40
0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4 2.6 2.8 3 3.2 3.4 3.6 3.8 4 4.2 4.4 4.6 4.8 5
Freq
uenc
y
Mass in Solar Masses
Mass Histogram
0
10
20
30
40
50
60
0.4
1.6
2.8 4
5.2
6.4
7.6
8.8 10
11.2
12.4
13.6
14.8
16
17.2
18.4
19.6
Δν
Histogram of Δν
Statistics
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HR Diagrams
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Surface Rotation
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* An iterative fitting routine where functions are fit over the time series. This produces a contour plot.
* Star must have some feature on its surface rotating in and out of view.
* Kepler is also a source of periodicity.
Wavelet Analysis
Example of a Morlet Function, sv.wikipedia.org/wiki/Fil:Wavelet_-‐_Morlet.png
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Example of the Sun
Image taken from Hempelman, 2003, A&A, 399, 717
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• Red contour shows the rotation.
• Cone of Influence shows where results are discarded. (These results could not have had repeated by the minimum of 4 times)
• Very wide contour implies differential rotation in the star.
• The graph of the periodicity shows that these features are dark.
Results
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• Data could be greatly improved with a longer time series, as the contours are very close to the cone of influence.
• 14/24 stars were found to have useful values of surface rotation ranging between 77 days and 137 days.
• Differential rotation is suggested by the width of the contour
• Much longer period for change in red giant stars, less detailed contours implying that the features aren’t changing so rapidly.
Results
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• Inclination: If the star is rotating around an axis that is inclined to the observer the rotation won’t be seen.
• Inactivity: Without star spots the rotation cannot be detected.
• Long Period Rotation: If red giants rotate with periods of more than a quarter of the observing time the findings are discounted.
• Satellite Effects
What affects surface rotation detection?
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• We have generated a pipeline that is 80% effective • We have shown the rotation of red giant stars is very
slow compared with solar like stars • We have shown that red giants are still active well
into late evolution. • Through studying surface rotation further of more
evolved stars it is possible to study the transport of angular momentum.
Conclusions
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