The Millisecond Pulsar Contribution to the Rising Positron Fraction Christo Venter 34 th ICRC, The...
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![Page 1: The Millisecond Pulsar Contribution to the Rising Positron Fraction Christo Venter 34 th ICRC, The Hague, The Netherlands, 30 July – 6 August 2015 Collaborators:](https://reader035.fdocuments.net/reader035/viewer/2022062806/5697bf7c1a28abf838c83d97/html5/thumbnails/1.jpg)
The Millisecond Pulsar Contribution to the Rising Positron Fraction
Christo Venter
34th ICRC, The Hague, The Netherlands, 30 July – 6 August 2015
Collaborators: AK Harding, A Kopp, PL Gonthier, I Buesching
(Venter et al. 2015a,b)
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• ~200 field MSPs– 160 binary
(80%)– 40 isolated
• 144 in globular clusters
• ~70 g-ray MSPs• Very different
characteristics from young PSRs– P = 1.5 –
~ 100 ms– B ~ 108 – 1010 G– T ~ 108 – 109 yr
• “Recycled” pulsars spun-up by binary companion stars
Recycled MSPs
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Credit: Scott Ransom
New MSP Discoveries
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Motivation
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Millisecond pulsars Young pulsars
Light curves of many MSPs show narrow peaks out of phase with radio peaks - indistinguishable from those of young pulsars
Narrow accelerator gaps
Screening by electron-positron pairs
Similar MSP and Young-Pulsar LCs
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Aguilar et al. (2013, 2014)
Rising positron fraction! Need primary e+ source(s)
Predicted secondary e+
from CR interactions
Recent CR Measurements
II
II
I?
I?
PF
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(Young) Pulsars as Sources of CRs
• E.g., nearby canonical pulsars producing e-e+ pairs.• OTHER sources: SNR, PWN, DM, …
Di Bernardo et al. (2009)
cf. Zhang & Cheng (2001), Grasso et al. (2009), Profumo (2008), Gendelev (2010)
What about MSPs?• No
surrounding nebula
• One layer of uncertainty removed.
• Data fitting• Bottom-up
model
Two approaches:
PF
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Summary: Motivation for Studying MSP Contribution• Many new MSP detections: larger number of
sources: NMSP
• Light curves point to copious pair production: larger number of particles per source: M+
• New black widows / redbacks: additional acceleration in shocks: hmax
• Simpler systems than young pulsars No surrounding PWN, removing uncertainty
in particle escape Old systems – steady-state approach Spherical symmetry of MSP spatial
distribution
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Model
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Galactic MSP Synthesis
Gonthier et al., in prep.
~50 000 MSPs in
the Galaxy
Venter et al. (2015a,b)
SOURCES
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Galactic MSP Synthesis
Gonthier et al., in prep.
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Harding & Muslimov (2011)
Need offset polar caps or non-dipolar fields for pair cascades in MSPs
Offset parameter e for MSPs:
0.0 – static dipole0.1 – vacuum dipole0.2 – force-free dipole> 0.2 – multipoles
Pair Death Lines for Offset PCsSPECTRA
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Consider two contributions:
1. Direct injection of pair spectra from pulsar magneto-spheres
2. Injection of pair spectra after acceleration in binary shock
Harding & Muslimov (2011a,b)
MSP Pair Cascade Spectra
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• MSPs with very low-mass binary companions– 10 – 80 Jupiter
masses (~0.01 M )
• Tight binaries (Pb < 24 h)
• Radio eclipses common
• Pulsar wind ablates companion by exciting stellar winds
• Redbacks (cousins)– ~0.1 M companions
.
.
Before Fermi’s launch: 3 black widows, 1 redbackNow: >18 black widows, 8 redbacks – Total >26!
Black Widows& Redbacks
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Shock acceleration spectrum
Maximum acceleration energy(Harding & Gaisser 1990)
NormalizationPair multiplicity PC flux
Efficiency
Particle Acceleration at the Binary Shock
Venter et al. (2015a,b)
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Kopp et al. (2013)
Pair injection spectrum
Spatial E-dependent diffusion (scalar here)
SR & IC losses with KN limit
Galactic background photons (CMB; IR; optical)
Steady state Spherical
symmetry Full transport
equation
Galactic CR Transport
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Results
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Venter et al. (2015b)
Galactic CR Transport: Losses
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Pair cascades
Binary shocks
Efficiency hp,max = 0.1 Efficiency hp,max = 0.3
• Pair cascades from magnetosphere contribute at lower energies
• Pairs accelerated in intra-binary shocks in Black Widow & Redback systems: larger contribution at high energies
e = 0
e = 0.2
e = 0.6
Venter et al. (2015b)
e+ and e- Spectra from MSPs
κ0 = 0.1 kpc2 Myr−1
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Pair cascades
Binary shocks
Efficiency hp,max = 0.1; κ0 = 0.1 kpc2 Myr−1
The effect of aD: Smaller value similar to smaller diffusion at high energies – pile-up effect
e = 0
e = 0.2e = 0.6
e+ and e- Spectra from MSPs
Venter et al. (2015b)
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Efficiency hp,max = 0.1 Efficiency hp,max = 0.3
e = 0
e = 0.2
e = 0.6
MSP Contribution to CR e+ and e- Spectra
κ0 = 0.1 kpc2 Myr−1Venter et al. (2015b)
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Lowering diffusion coefficient by a factor of ten increases contribution – pile-up effect
e = 0
e = 0.2
e = 0.6
Efficiency hp,max = 0.1 Efficiency hp,max = 0.3
MSP Contribution to CR e+ and e- Spectra
κ0 = 0.01 kpc2 Myr−1Venter et al. (2015b)
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Different values of aD
e = 0
e = 0.2
e = 0.6
Efficiency hp,max = 0.1 κ0 = 0.1 kpc2 Myr−1
MSP Contribution to CR e+ and e- Spectra
Venter et al. (2015b)
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e = 0
e = 0.6
MSP Contribution to Positron Fraction
e = 0.2
Efficiency hp,max = 0.1 Efficiency hp,max = 0.3
κ0 = 0.1 kpc2 Myr−1Venter et al. (2015b)
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e = 0e = 0.6
Lowering diffusion coefficient by a factor of ten increases contribution – pile-up effect
MSP Contribution to Positron Fraction
Efficiency hp,max = 0.1 Efficiency hp,max = 0.3
e = 0.2
κ0 = 0.01 kpc2 Myr−1Venter et al. (2015b)
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e = 0
e = 0.6
MSP Contribution to Positron Fraction
Efficiency hp,max = 0.1 κ0 = 0.1 kpc2 Myr−1
e = 0.2
Different values of aD
Venter et al. (2015b)
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e = 0
e = 0.6
Different ‘background model’: Delahaye et al. (2010)
MSP Contribution to Positron Fraction
Efficiency hp,max = 0.1 Efficiency hp,max = 0.3
e = 0.2
k0 = 0.1 kpc2 Myr-1 k0 = 0.01 kpc2 Myr-1
Venter et al. (2015b)
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Conclusions
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• Different realizations for Synthesis Population
• Limits on source parameters• Contribution of other secondary
sources• Primary / secondary contributions• Isotropy vs. pulsar origin of CR excess• Implications of Galactic Centre g-ray
excess
Points for Discussion
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• MSP pair cascades make up to ~ 15% contribution to CR positrons at 10 – 100 GeV, depending on background model
• Pairs accelerated in intra-binary shocks could make a significant contribution to positron fraction up to several TeV
• With the growing population of black widows and redbacks, present estimate is a lower limit
Conclusions
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THANK YOU!
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