Pulsar High Energy Emission Models: What Works and What Doesn't

Pulsar High Energy Emission Models: What Works and What Doesn't

• “Standard” outer magnetosphere models - successes

• Shortcomings of the models

• Next steps?

Alice K. HardingNASA Goddard Space Flight Center

“Standard” outer magnetosphere models - successes

“Standard” outer magnetosphere models - successes

• Outer gap, slot gap and separatrix layer models can roughly produce observed gamma-ray light curves – but require thin emission layers

• Predicted cutoff energies for curvature radiation roughly match observed cutoff energies

• Variation of curvature radius similar to phase resolved cutoff energies

Pulsar accelerator geometriesPulsar accelerator geometriesPulsar accelerator geometriesPulsar accelerator geometries

€

γγ→ e±

€

γ→ e±

pair-starvedpolar cap

slotgap / TPC

Accelerator GeometriesAccelerator GeometriesAccelerator GeometriesAccelerator Geometries

Narrow accelerators require screening of E field by pairs

Narrow accelerators require screening of E field by pairs

Caustic emissionCaustic emission• Photons emitted parallel to Photons emitted parallel to

dipole magnetic fielddipole magnetic field• Aberration and time-of-flight Aberration and time-of-flight

delaysdelays• Trailing outer edge of open Trailing outer edge of open

volumevolume

Caustic emissionCaustic emission• Photons emitted parallel to Photons emitted parallel to

dipole magnetic fielddipole magnetic field• Aberration and time-of-flight Aberration and time-of-flight

delaysdelays• Trailing outer edge of open Trailing outer edge of open

volumevolume

Emission on trailing field Emission on trailing field lineslines

• Bunches in phaseBunches in phase• Arrives at inertial Arrives at inertial

observer observer simultaneouslysimultaneously

Emission on trailing field Emission on trailing field lineslines

• Bunches in phaseBunches in phase• Arrives at inertial Arrives at inertial

observer observer simultaneouslysimultaneously

Emission on leading field Emission on leading field lineslines

• Spreads out in phaseSpreads out in phase• Arrives at inertial Arrives at inertial

observer at different observer at different timestimes

Emission on leading field Emission on leading field lineslines

• Spreads out in phaseSpreads out in phase• Arrives at inertial Arrives at inertial

observer at different observer at different timestimes

Formation of causticsFormation of causticsFormation of causticsFormation of caustics

Slot gap

Outer gap

= 300 = 600 = 900

Sky distribution of intensitySky distribution of intensitySky distribution of intensitySky distribution of intensity

Phase

Observer angle

Phase

Light curves in force-free geometryLight curves in force-free geometryLight curves in force-free geometryLight curves in force-free geometry

Bai & Spitkovsky 2010

Young Radio-loud PulsarsYoung Radio-loud Pulsars

9

PSR J1028-5819 (Abdo et al., ApJL 695, 72, 2009)

PSR J2021+3651 (Abdo et al., ApJ 700, 1059, 2009)

PSR J0205+6449 (Abdo et al., ApJL 699, 102, 2009)PSR J1048-5832 & J2229+6114 (Abdo et al., ApJ 2009 accepted)

PSR J1420-6048 (Weltevrede et al., ApJ 2009 submitted)

16 Pulsars Found in Blind 16 Pulsars Found in Blind SearchesSearches

After 4 months of data taking, 16 pulsars were found with blind search technique!(Abdo et al., Science 325, 840, 2009).

13 were unidentified sources for EGRET

Radio-loud millisecond pulsarsRadio-loud millisecond pulsars

Fermi LAT detected pulsed gamma-Fermi LAT detected pulsed gamma-ray emission from J0030+0451, ray emission from J0030+0451, making it the first firm detection of an making it the first firm detection of an MSP in gamma rays (Abdo et al., ApJ MSP in gamma rays (Abdo et al., ApJ 699, 1171, 2009).699, 1171, 2009).

After 9 months of data taking, the LAT After 9 months of data taking, the LAT had detected 8 gamma-ray MSPs had detected 8 gamma-ray MSPs (Abdo et al. Science 325, 848, 2009).(Abdo et al. Science 325, 848, 2009).

For the first time, a population of For the first time, a population of gamma-ray MSPs has been gamma-ray MSPs has been observed.observed.

10

PSR J0034-0534

Modeling young pulsar light curvesModeling young pulsar light curvesModeling young pulsar light curvesModeling young pulsar light curves

(, , w) = (73, 53, 0.07)

Decesar et al., in prep.

TPC

Off-peak emission too high

(, , w) = (68, 26, 0.05)

TPC

Modeling MSP Light CurvesModeling MSP Light CurvesModeling MSP Light CurvesModeling MSP Light Curves

OGTPC~ 0.45~ 0.45

~ 0.16~ 0.16

OG1 (80,70)

TPC1 (70,80)

= 70o, P = 5 ms

γ-ray

Radio

PSR J0030+0451PSR J0030+0451

Venter, Harding & Guillemot 2009

PSR J0613-0200PSR J0613-0200PSR J0613-0200PSR J0613-0200

OGTPC

OG1 (30,60)

TPC2 (30,60)

Radio

= 30= 3000, , = 60 = 6000

Radio 1400 MHz

Radio 1400 MHz

γ-ray

Predicted CR cutoff energies roughly match observed cutoff energies

Balance CR losses with acceleration gain

Steady-state Lorentz factor

Curvature radiation peak energy:

€

εCR =2

3

λ cγCRR3

ρ c

=3

2

⎛

⎝ ⎜

⎞

⎠ ⎟7 / 4

E ||

e

⎛

⎝ ⎜

⎞

⎠ ⎟3 / 4

λ cρ c1/ 2 ≈ 3 GeV

1/ 42|| 73

2 102

cCRR

E

e

γ

€

eE|| = ˙ γ CR =2e2γ 4

3ρ c2

€

E || ~ w2BLC

Observed cutoff energies show remarkably small spreadObserved cutoff energies show remarkably small spread

Phase resolved cutoff energiesVela

Geminga

J1836+5925CTA1

Emission radius

Curvature radius

Light curve

= 700

Model variation of emission, curvature Model variation of emission, curvature radiusradiusDeCesar et al., in prep.

Shortcomings of the modelsShortcomings of the models• Energetics

too small for both slot gap and outer gap models by a factor of 5 – 10 (for narrow gap widths)

• Lack of sufficient pairs –

for either PWNe: Crab nebula requires ~1040 s-1 particles pair multiplicity ~ 106

or MSPs with narrow gaps emission

• Dipole field geometry and lack of current closure

€

Lγ = ˙ n γmc 2

near the surfacenot efficient screening

Ne2/Ne1 = 10-3-102

Sturner & Dermer ‘94Hibschmann & Arons ’01

higher above the surfaceE// screening

Ne2/Ne1 = 10-105

Daugherty & Harding ’82

Zhang & Harding ‘00

e (1-10 TeV)

CRCR< 50 GeV< 50 GeVCRCR< 50 GeV< 50 GeV

SYNSYN

ICSICS

e±

X(surface)X(surface)

X(surfacesurface)

ICSICS

SYNSYNe±

e±

e±

e±

e±

e (0.05-500 GeV)

γ + B eγ + B e

Polar cap pair cascadesPolar cap pair cascadesPolar cap pair cascadesPolar cap pair cascades

Pulsar pair cascadesPulsar pair cascadesPulsar pair cascadesPulsar pair cascadesPolar cap pair death linesPolar cap pair death lines

Harding & Muslimov 2002, Harding et al. 2005

PC cascade pair spectrumPC cascade pair spectrum

Pair energies can reach 100 GeV Pair energies can reach 100 GeV

Cascade pair multiplicityCascade pair multiplicity

Above/below CR pair death line – high/low pair multiplicity (for dipole field)Above/below CR pair death line – high/low pair multiplicity (for dipole field)

High pair multiplicityHigh pair multiplicity

Low pair multiplicityLow pair multiplicity

What about millisecond pulsars?What about millisecond pulsars?• Many detected by Fermi• Pair cascades in dipole fields not expected to have high

multiplicity ‘pair starved’• But gamma-ray light curves show narrow peaks, not in phase

with radio narrow acceleration gaps

Field geometry and current closureField geometry and current closure

• Emission models assume retarded vacuum dipole field

• Emission models ignore current closure

• Force-free current is not the same as GJc assumed by models

Force-free magnetosphereSpitkovsky 2008

Bai & Spitkovsky 2010

NS SURFACE

e+

i+

e-

e-

Next steps• Understand acceleration in self-consistent global geometry?

(not likely anytime soon!)• Accelerate both signs of charge above polar cap?

e-

e+

• Space-charge limited ion (as well as electron)acceleration

• Lorentz-boosted pair production(Cheng & Ruderman 1977)

• Positrons initiate pair cascade

QuestionsQuestions

• How do MSPs (and maybe all pulsars) produce higher pair multiplicities?

• How do polar cap pair cascades link to global magnetosphere currents (and what happens when pulsars are pair-starved)?

• How do thin gaps produce observed gamma-ray luminosity?