SEARCHING FOR MAGNETIC ACTIVITY IN SOLAR-LIKE STARS OBSERVED BY KEPLER
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1 SEARCHING FOR MAGNETIC ACTIVITY IN SOLAR-LIKE STARS OBSERVED BY KEPLER Lauren Balliet Clarion University of Pennsylvania Space Science Institute : Savita Mathur LASP National Science Foundation
2 IMPORTANCE Solar magnetic activity are not completely understood Better understanding of our own sun
3 IMPORTANCE CONTINUED Study other stars with different conditions in order to have a broader vision New interpretations for dynamo models of solar -like stars Magnetic cycles rotation, convection, and magnetic field in solar like stars
4 WHAT WE KNOW OF MAGNETIC ACTIVITY IN SOLAR-LIKE STARS Spectroscopy Surveys Mount Wilson [Wilson 1978, Baliunas et al 1995] Lowell Observatory [Hall 2007] The Sun In a transition stage [Metcalfe et al. 2016] HD49933 i Horologii [Bohm-Vitense, 2007]
5 GOAL Determine if there are any magnetic activity cycles are present in a data set of 540 pulsating solar like stars that were observed by Kepler. [Chaplin et al.2011]
6 KEPLER March 6, 2009 Four years of continuous photometric data ~200,000 stars Main Goal 2327 exoplanets Stellar Physics Asteroseismology
7 KEPLER OBSERVATIONS Long Cadence ~30 minutes Short Cadence ~60 seconds Data Transfer ~30 days Rotates 90 3 months Quarters in the data: Q17 total
8 LIGHT CURVE Calibration to correct for instrument issues [Garcia et al. 2011] Jumps / outliers / trends
9 ROTATION PERIOD Analyzed 540 stars to look for surface rotation period Active Star have spots Change in flux Analysis done by Garcia et al stars Data up to Q14 [Garcia et al ]
10 DETERMINATION OF ROTATION PERIOD Techniques [Periodogram] Auto Correlation Time Frequency Reliability of results Comparison to Garcia et al Visual Check
11 DETERMINATION OF ROTATION PERIOD Techniques [Periodogram] Auto Correlation Time Frequency Reliability of results Comparison to Garcia et al Visual Check Duplicate for Animation
12 WHAT DID WE FIND? There were 304 stars with reliable rotation periods found. Number of Stars versus Period of Rotation
13 GARCIA COMPARISON 13 stars were found outside of Garcia et al KIC KIC
14 MAGNETIC ACTIVITY Magnetic Proxy (Sph) Standard Deviation of the Subseries of Length = k x Prot Wavelet Power Spectrum Scale Average (+/- 20% Prot) k=3
15 S PH AND SCALE AVERAGE CORRELATION The S ph and the Scale Average show a direct correlation 400 KIC S ph (ppm) Time (days) Scale Average (1x10 4 ) Time (days) Differences could result from different time scales Correlation :
16 CANDIDATES Visual check Cycle, Steady Power, Trend, Variable, Burst, Not Sure 15 Cycle Candidates KIC
17 CANDIDATES Visual check Cycle, Steady Power, Trend, Variable, Burst, Not Sure 15 Cycle Candidates KIC Duplicate for Animation
18 CYCLE CANDIDATES KIC T eff Mass Gravity Rotation Period 6917 K M dex 12.5 days
19 CYCLE CANDIDATE KIC T eff Mass Gravity Rotation Period 6137 K M dex 1.4 days
20 CYCLE CANDIDATES Shere-Khan KIC T eff Mass Gravity Rotation Period 6676 K M dex 2.5 days
21 CANDIDATE RESULTS 4 P rot vs P cycle 3 P cycle (yr) P rot (days) Mass Ranges : 0.98 to 1.50
22 CANDIDATE RESULTS 4 P rot vs P cycle 3 P cycle (yr) P rot (days) HD49933 i Horologii [Bohm-Vitense, 2007] Mass Ranges : 0.98 to 1.50 Duplicate for Animation
23 ASTEROSEISMOLOGY Study the internal structure and dynamics of the Sun and other stars Two main types of oscillations modes Gravity modes Acoustic modes Pressure driven modes are acoustic waves for which the restoring force arises from the pressure gradient
24 SUN S ACOUSTIC MODES We know how the modes are changing when magnetic activity is changing Number of Sun Spots [Garcia et al. 2010]
25 SUN S ACOUSTIC MODES We know how the modes are changing when magnetic activity is changing HD49933 F5V star 20% more massive than the Sun 34% larger than the Sun [Garcia et al. 2010] Duplicate for Animation
26 ANTI CORRELATION OF ACOUSTIC MODES Anti-correlation between magnetic activity and amplitude of the modes by correlating with the S ph and Scale Average Subseries of 180 days Shifted by 30 days Amplitudes of the modes computed with A2Z Pipeline [Mathur et al. 2010] Power Spectrum (ppm 2 /μhz) Frequency (μhz)
27 COMPARISON TO S PH AND SCALE AVERAGE Star with Trend A maxx (ppm) KIC Time (days) Scale Average (1x10 4 ) S ph (ppm) Time (days) Time (days) S ph Correlation : Scale Average Correlation :
28 COMPARISON TO S PH AND SCALE AVERAGE Star with Magnetic Cycle S ph Correlation : Scale Average Correlation :
29 CONCLUSION 304 stars with reliable rotation periods 15 candidates they exhibit magnetic cycle like features 13 show anti-correlation between acoustic modes amplitude and S ph and Scale Average 3 of the cycle candidates show anti-correlation Frequency shifts analysis Stellar Modeling to infer the structure in combination with stellar dynamo model Propose to have spectroscopic observations to have a full analysis
30 THANK YOU Acknowledgements : National Science Foundation REU grant to the University of Colorado LASP REU Program Marty Snow and Erin Wood Space Science Institute Savita Mathur My fellow REU students
31 QUESTIONS?
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