154 MHz detection of faint, polarised flares from UV Ceti
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1 154 MHz detection of faint, polarised flares from UV Ceti Christene Lynch University of Sydney/CAASTRO Collaborators: Emil Lenc, University of Sydney/CAASTRO Tara Murphy, University of Sydney/CAASTRO David Kaplan, University of Wisconsin Milwaukee Gemma Anderson, Curtin University
2 Stellar Flares Flaring is a common characteristic of magnetically active stars. Observations of stellar flares: Provide constraints on stellar magnetic properties Solar - Stellar connection Habitability of discovered exoplanets
3 MHz Stellar flares Spangler et al. (1976) Single dish observations (1960 s s) measured: Flare rates = flares/hour Duration = hours Intensities = Jy Possible association with optical flares Non-detections in MWA blind surveys for transients: Tingay et al. (2016): Kepler K2 field, 5.9 hours Rowlinson et al. (2016): 100 hrs of MWA EoR field
4 MHz Stellar flares Spangler et al. (1976) Single dish observations (1960 s s) measured: Flare rates = flares/hour Duration = hours Intensities = Jy Possible association with optical flares Non-detections in MWA blind surveys for transients: Tingay et al. (2016): Kepler K2 field, 5.9 hours Rowlinson et al. (2016): 100 hrs of MWA EoR field Where are all the flare stars?
5 Coherent Emission At <5 GHz emission dominated by coherent mechanism: 2 possible types 1. Electron Cyclotron Maser Emitted at local fundamental/2nd harmonic cyclotron frequency: νc ~ 2.8 MHz (BGauss) Constrain B-field Confirmed emission mechanism for radio bursts of brown dwarfs 2.Plasma Emission Emitted at local fundamental/2nd harmonic plasma frequency: νp ~ 9.0 khz (ncm -3 ) 1/2 Constrain Density Different types of Solar flares due to plasma emission NOTE: Coherent emission expected to be highly (>50%) circularly polarised!
6 MWA Observations UV Ceti: Spectral types = dm5.5e Binary system w/ 26 yr period both exhibit radio flares Distance = 2.7 pc Pointed observations phase center moved to keep source within primary beam Total observation time = 8.8 hours split over 4 days in Dec 2015 Frequency = 154 MHz; bandwidth MHz
7 Detection of UV Ceti December : 30 min integrations 1σ RMS = 80 mjy 1σ RMS = 1 mjy Lynch et al. (submitted to ApJ)
8 Light-curve analysis STOKES V (pos = RH, neg = LH) PERIODICITY: Mid-flare time & amplitudes fit using tophat function (only RH) Minimize phase difference for set of trial periods P = ± hrs (95% confidence) v sin(i) ~ 30 km/s -> P < 6.5 hrs Lynch et al. (submitted to ApJ)
9 Emission Type? 1. Brightness Temperature: A. Source size constrained by assuming periodic persistent source: L = Δt vsin(i) ~ 10 9 cm Tb ~ K
10 1. Brightness Temperature: Emission Type? A. Source size constrained by assuming periodic persistent source: L = Δt vsin(i) ~ 10 9 cm Tb ~ K B. Source size constrained by VLBA: L~10 10 cm Tb ~10 13 K Benz et al cm
11 Emission Type? 1. Brightness Temperature: Tb ~ ( ) K Coherent Lynch et al. (submitted to ApJ)
12 Emission Type? 1. Brightness Temperature: Tb ~ ( ) K Coherent 2.Polarisation: A. Circular: Both right & left handed; >27% B. Linear: >18%; ϕ = + 3 rad m -2 Lynch et al. (submitted to ApJ)
13 Emission Type? 1. Brightness Temperature: Tb ~ ( ) K Coherent 2.Polarisation: A. Circular: Both right & left handed; >27% B. Linear: >18%; ϕ = + 3 rad m Time/Frequency structure: A. For 6-min/10 MHz bins, constant across full MHz bandwidth B. Due to low SNR cannot rule out finer structure
14 Emission Type? 1. Brightness Temperature: Tb ~ ( ) K Coherent 2.Polarisation: A. Circular: Both right & left handed; >27% B. Linear: >18%; ϕ = + 3 rad m Time/Frequency structure: A. For 6-min/10 MHz bins, constant across full MHz bandwidth B. Due to low SNR cannot rule out finer structure 4. Optical/X-ray counterpart: A. No optical coverage during MWA observations B. Both Swift Burst Alert & Monitor of All-sky X-ray Image monitor UV Ceti; no bright X-ray flares detected
15 Emission Type? 1. Brightness Temperature: Tb ~ ( ) K Coherent 2.Polarisation: A. Circular: Both right & left handed; >27% B. Linear: >18%; ϕ = + 3 rad m Time/Frequency structure: A. For 6-min/10 MHz bins, constant across full MHz bandwidth B. Due to low SNR cannot rule out finer structure 4. Optical/X-ray counterpart: A. No optical coverage during MWA observations B. Both Swift Burst Alert & Monitor of All-sky X-ray Image monitor UV Ceti; no bright X-ray flares detected Cannot determine type of emission
16 MHz Flare rates Lynch et al. (submitted to ApJ)
17 Summary & Future work: 1. Observed 4 flares from M dwarf UV Ceti during 8.8 hr observation 2. Flares only detected in Stokes V images due to order of magnitude higher noise in confusion limited Stokes I images. 3. Flares are coherent but cannot distinguish between different emission types. Need wider bandwidths, higher sensitivity, and multi-wavelengths. 4. First flare rates for low intensity (<100 mjy) flares at MHz consistent with previous (brighter) detected flares. NEXT STEPS: 1. Detect more stellar flares! Target larger sample of M dwarfs with similar observational scheme (LST align observations) 2. Use results to constrain flare rates & coordinate multi-wavelength shadowing
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