Preparing to re-visit the inner heliosphere

David Stansby

+ Tim Horbury, Chadi Salem, Lorenzo Matteini, Denise Perrone

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Download these slides atdavidstansby.com/talks

The Solar Wind

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DeForest et al. 2018

15r⊙

LASCO/C2(Solar max)

Open questions

• In-situ measurements at 1 AU limited by processes that erase information on source regions during transit

• To mitigate this, get close to the Sun → SO and PSP

• But we have been to the inner heliosphere before!

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“Trying to answer Solar Orbiter and Parker Solar Probe science objectives before they launch”

Measurements inside 1 AU

• Helios have the only comprehensive, archived in-situ measurements of the inner heliosphere to date

• Reprocessed to provide reproducible + reliable proton number densities, speeds, and temperatures (Stansby 2018, arXiv)

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Mariner 2: Neugebauer et al. 1962; MESSENGER: Gershman et al. 2012

In-situ measurements

• All in-situ spacecraft typically measuremagnetic field & proton velocity distribution function

• Derive number density, velocity, and temperatures

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Stansby et al. 2018

(times 2,000,000)

Rest of talk structure

• For each topic I’ll give

• Overview of relevant remote sensing measurements

• What we have learnt from Helios measurements

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1. Coronal hole jets

2. Solar wind source regions

3. Coronal heating mechanisms

Solar coronal jets

• x

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See Raouafi et al. 2016 for a review

Sterling et al. 2015

Solar coronal jets

• Occur almost everywhere

• Easy to spot in coronal holes due to dark background

• Are there signatures of jets in the solar wind?

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Roberts et al. 2018vp

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Fast solar wind

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1 AU

0.3 AU

10 days

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(See Matteini et al. 2015 for details)

Fast solar wind

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30 minutes

After Horbury et al. 2018

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Fast solar wind

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30 minutes

• Alfvénic ‘jets’ occur almost everywhere in the fast solar wind

• Much faster closer to the Sun (�v / vA)<latexit sha1_base64="8x/NBKEnKC4xlBoJw1kGm/OxPwI=">AAACCnicbVC7TsMwFHXKq5RXgJHFUCGVpUoQEowFFsYi0YfURJHjOK1Vx4lsp1IVZWbhV1gYQIiVL2Djb3DaDNByJEtH59wr33P8hFGpLOvbqKysrq1vVDdrW9s7u3vm/kFXxqnApINjFou+jyRhlJOOooqRfiIIinxGev74tvB7EyIkjfmDmibEjdCQ05BipLTkmccNJyBMIehESI38MJvk0ElEnKgYTrzsOj/zzLrVtGaAy8QuSR2UaHvmlxPEOI0IV5ghKQe2lSg3Q0JRzEhec1JJEoTHaEgGmnIUEelmsyg5PNVKAMNY6McVnKm/NzIUSTmNfD1ZHCwXvUL8zxukKrxyM8qTVBGO5x+FKYM6Z9ELDKggWLGpJggLqm+FeIQEwkq3V9Ml2IuRl0n3vGlbTfv+ot66KeuogiNwAhrABpegBe5AG3QABo/gGbyCN+PJeDHejY/5aMUodw7BHxifP9OLmlY=</latexit><latexit sha1_base64="8x/NBKEnKC4xlBoJw1kGm/OxPwI=">AAACCnicbVC7TsMwFHXKq5RXgJHFUCGVpUoQEowFFsYi0YfURJHjOK1Vx4lsp1IVZWbhV1gYQIiVL2Djb3DaDNByJEtH59wr33P8hFGpLOvbqKysrq1vVDdrW9s7u3vm/kFXxqnApINjFou+jyRhlJOOooqRfiIIinxGev74tvB7EyIkjfmDmibEjdCQ05BipLTkmccNJyBMIehESI38MJvk0ElEnKgYTrzsOj/zzLrVtGaAy8QuSR2UaHvmlxPEOI0IV5ghKQe2lSg3Q0JRzEhec1JJEoTHaEgGmnIUEelmsyg5PNVKAMNY6McVnKm/NzIUSTmNfD1ZHCwXvUL8zxukKrxyM8qTVBGO5x+FKYM6Z9ELDKggWLGpJggLqm+FeIQEwkq3V9Ml2IuRl0n3vGlbTfv+ot66KeuogiNwAhrABpegBe5AG3QABo/gGbyCN+PJeDHejY/5aMUodw7BHxifP9OLmlY=</latexit><latexit sha1_base64="8x/NBKEnKC4xlBoJw1kGm/OxPwI=">AAACCnicbVC7TsMwFHXKq5RXgJHFUCGVpUoQEowFFsYi0YfURJHjOK1Vx4lsp1IVZWbhV1gYQIiVL2Djb3DaDNByJEtH59wr33P8hFGpLOvbqKysrq1vVDdrW9s7u3vm/kFXxqnApINjFou+jyRhlJOOooqRfiIIinxGev74tvB7EyIkjfmDmibEjdCQ05BipLTkmccNJyBMIehESI38MJvk0ElEnKgYTrzsOj/zzLrVtGaAy8QuSR2UaHvmlxPEOI0IV5ghKQe2lSg3Q0JRzEhec1JJEoTHaEgGmnIUEelmsyg5PNVKAMNY6McVnKm/NzIUSTmNfD1ZHCwXvUL8zxukKrxyM8qTVBGO5x+FKYM6Z9ELDKggWLGpJggLqm+FeIQEwkq3V9Ml2IuRl0n3vGlbTfv+ot66KeuogiNwAhrABpegBe5AG3QABo/gGbyCN+PJeDHejY/5aMUodw7BHxifP9OLmlY=</latexit><latexit sha1_base64="8x/NBKEnKC4xlBoJw1kGm/OxPwI=">AAACCnicbVC7TsMwFHXKq5RXgJHFUCGVpUoQEowFFsYi0YfURJHjOK1Vx4lsp1IVZWbhV1gYQIiVL2Djb3DaDNByJEtH59wr33P8hFGpLOvbqKysrq1vVDdrW9s7u3vm/kFXxqnApINjFou+jyRhlJOOooqRfiIIinxGev74tvB7EyIkjfmDmibEjdCQ05BipLTkmccNJyBMIehESI38MJvk0ElEnKgYTrzsOj/zzLrVtGaAy8QuSR2UaHvmlxPEOI0IV5ghKQe2lSg3Q0JRzEhec1JJEoTHaEgGmnIUEelmsyg5PNVKAMNY6McVnKm/NzIUSTmNfD1ZHCwXvUL8zxukKrxyM8qTVBGO5x+FKYM6Z9ELDKggWLGpJggLqm+FeIQEwkq3V9Ml2IuRl0n3vGlbTfv+ot66KeuogiNwAhrABpegBe5AG3QABo/gGbyCN+PJeDHejY/5aMUodw7BHxifP9OLmlY=</latexit>

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Jet conclusions

• Jets may have important role in heating coronal hole wind

• No in-situ indications of heating/density enhancements

• See Horbury et al. 2018 for more details on Helios work

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Solar wind sources

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• Try to categorise in-situ solar wind measurements into different sources

• Been attempted before (e.g. Neugebauer et al. 2017), but only with 1 AU data

• Possible sources are

• Coronal holes (centre + edges)

• Active regions (e.g. Harra et al. 2017)

• Small transients (e.g. Sheeley et al. 1997)

Cutting by speed doesn’t work

• All fast solar wind is a smooth flow + Alfvén waves

• Recent work has found similar (lack of) structure within slow wind (D’Amicis et al. 2015, 2016)

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1 day

vr

vt

Bt

• Alfvénicity might be a more fundamental variable(related to open/closed field)

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1 hour

vr

vt

Bt

np

Cutting by speed doesn’t work

Radial variation of Alfvénicity

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Alfvénicnon-Alfvénic

0.3 AU

1 AU• All Helios data at solar

minimum

• Properties at 1 AU not reflective of solar source properties!

50%50%

80%20%

Alfvénic wind at 0.3 AU

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‘Alfvénicity’

Classification timeseries

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20 Days

Using T⟂/T|| to infer composition

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“Entropy”

• Ulysses and ACE show entropy andO7+/O6+are statistically correlated[Pagel et. al. 2004, Stakhiv et. al. 2015, 2016]

• Also sharp O7+/O6+ boundaries at leading + trailing edges of high speed streams [Burton et. al. 1999, Borovsky et. al. 2016]

• Helios saw sharp anisotropy boundaries in the leading and trailing edges at 0.3 AU

Low coronal temp

High coronal temp

Classification timeseries

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20 Days

Low Tc Low Tc High TcHigh TcHigh Tc

Speed + mass flux of the 3 categories

• Distinction between slow/fast blurred at intermediate speeds

• Alfvénic wind has steady mass flux →continuous release on open field lines

• Non-Alfvénic wind has varying mass flux → transient release on closed lines

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Iso Non-Alfvénic

Iso Alfvénic

Aniso Alfvénic

Categorisation conclusions

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Coronal holes • Low coronal temp • Constant mass flux • Includes high speeds

Active regions/CH edges • High coronal temp • Alfvénic + constant mass flux ⇒ quasi-steady open flux

Small transients • High coronal temp • non-Alfvénic +

variable mass flux ⇒ intermittent source

• Lots (~80 %) of slow wind is Alfvénic at 0.3 AU

• Solar wind at looks significantly different at 0.3 AU compared to 1 AU

• A prediction of contributions of different sources to the solar wind (at solar minimum)

Stansby et al. in prep

Coronal heating

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• One line of attack: see how heating affects different ions

• In-situ measurements of heavy ions only at > 1 AU (until SO)(e.g. Tracey et al. 2016)

• Remote sensing of lots of different ions(SOHO/UVCS, Hinode/EIS, e.g. Hahn et al. 2013, Cranmer et al. 2008)

Preferential heating

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SOHO/UVCS; Cranmer et al. 2017

Heaving ion heating Perpendicular heating

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SOHO/UVCS; Telloni et al. 2007

O5+

Fast wind He2+ at 0.3 AU

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Protons

Alphas

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• He2+ does undergo preferential heating…

• … but is less anisotropic than protons

• An important new constraint for coronal heating theories?

Work in progress

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• He2+ anisotropy << proton anisotropy

• He2+ becomes unstable ~ 0.3 AU

• He2+ properties at1 AU very strongly influenced by transit effects

Fast wind He2+ at 0.3 AU

Alphas

Protons

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10010-110-2

Work in progress

Conclusions

• Properties measured in-situ at 1 AU may not reflect solar sources

• Helios data are very valuable and still returning surprises

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• Developed testable scheme for categorising solar sources

• Trying to do science w/ Helios data has been excellent preparation for Parker Solar Probe and Solar Orbiter

Active regionsTransients

Coronal holes

Download these slides atdavidstansby.com/talks

Bibliography

• New Helios data - Stansby 2018(http://arxiv.org/abs/1807.04376)

• MESSENGER solar wind - Gershmann 2012(http://doi.wiley.com/10.1029/2012JA017829)

• Coronal jet review - Raouafi+ 2016 (http://link.springer.com/10.1007/s11214-016-0260-5)

• In-situ jets - Horbury+ 2018(https://academic.oup.com/mnras/article-abstract/478/2/1980/4987231)

• Solar wind movies - DeForest+ 2018 (http://iopscience.iop.org/article/10.3847/1538-4357/aac8e3)

• Alfvénic slow wind - D’Amicis+ 2015 (http://stacks.iop.org/0004-637X/805/i=1/a=84)

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