Monthly Proton Flux Monthly Proton Flux Matteo Palermo (University - - PowerPoint PPT Presentation

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Monthly Proton Flux Monthly Proton Flux Matteo Palermo (University - - PowerPoint PPT Presentation

Dec 02, 2023 401 likes •836 views

Properties of The Forbush Properties of The Forbush decreases measured by AMS decreases measured by AMS on the ISS on the ISS Monthly Proton Flux Monthly Proton Flux Matteo Palermo (University of Hawaii) on behalf of the AMS Collaboration

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Monthly Proton Flux Monthly Proton Flux

Properties of The Forbush Properties of The Forbush decreases measured by AMS decreases measured by AMS

  • n the ISS
  • n the ISS

Physics and Astronomy Department University of Hawaii at Manoa Honolulu, Hawaii, US

Matteo Palermo (University of Hawaii)

  • n behalf of the AMS Collaboration
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AMS Collaboration AMS Collaboration

UHM

AMS was installed on the International Space Station

  • n May 19, 2011

In 6 years of operation, AMS has measured over 100 billion events. It will continuously take data for the entire duration of the ISS

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Particle Identification with AMS Particle Identification with AMS

AMS is a general purpose detector which measures particles

in the GV-TV rigidity range

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Cosmic Rays (CR) Cosmic Rays (CR) Nuclei with AMS Nuclei with AMS

AMS measures all CR species with error at % level up to Fe and above It will improve our knowledge of CR sources, acceleration mechanisms and propagation More details in ICRC 2017 CR-D session: A. Oliva, Q. Yan, V. Choutko

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Proton and He Monthly Fluxes Proton and He Monthly Fluxes

At low rigidities, not only long-term solar modulation but also short-term solar activity

ICRC 2017 CR-D session : presentation from C. Consolandi Highlight talk by V. Bindi

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AMS Daily Proton Flux AMS Daily Proton Flux

Preliminary Data Please refer to the AMS forthcoming publication in PRL

June 21, 2015

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AMS observed fast decreases in the daily proton flux

AMS Daily Proton Flux AMS Daily Proton Flux

June 23, 2015

Preliminary Data Please refer to the AMS forthcoming publication in PRL

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Decreases may last several days

AMS Daily Proton Flux AMS Daily Proton Flux

June 27, 2015

Preliminary Data Please refer to the AMS forthcoming publication in PRL

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AMS Daily Proton Flux AMS Daily Proton Flux

This decrease lasted for 17 days

June 30, 2015

Preliminary Data Please refer to the AMS forthcoming publication in PRL

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AMS Daily Proton Flux AMS Daily Proton Flux

Gradually AMS proton flux recovers to previous conditions

July 7, 2015

Preliminary Data Please refer to the AMS forthcoming publication in PRL

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➢ Temporary decreases in the CR flux, followed by gradual recovery ➢ Often associated to passing of Interplanetary Coronal Mass Ejections (CME) and/or

Corotating Interacting Regions (CIR)

➢ Some of them may be associated with the arrival of Solar Energetic Particles (SEP)

accelerated at the Sun during CME or solar flares.

Forbush Decreases (FD) Forbush Decreases (FD)

March 2012 Solar Energetic Particle and Forbush decrease event

Preliminary Data Please refer to the AMS forthcoming publication in PRL Highlight talk by V. Bindi

1.02-1.10 GV 3.14-3.41 GV 5.09-5.52 GV 10.51-11.39 GV 20.00-21.68 GV

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FDs and SEPs FDs and SEPs

Highlight talk by V. Bindi

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➢ Although FDs can be seen also on the ground (e.g by Neutron Monitors),

the rigidity spectra of FDs and their time evolution are not precisely known

➢ The relationship with disturbances measured in the solar wind and FD behavior in rigidity

is unknown

➢ Remove the short-term effects to better study the long-term solar modulation

Why studying FDs with AMS? Why studying FDs with AMS?

March 2012 Solar Energetic Particle and Forbush decrease event

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Forbush Decreases Forbush Decreases Identification Identification

Characterize the day-to-day variability on AMS proton flux for each rigidity bin

  • 1. Select quiet periods (~ 1 month)
  • 2. Normalize the daily flux to the average of the first 3 days
  • 3. Calculate standard deviation (SD) of the daily flux distribution

Preliminary Data Please refer to the AMS forthcoming publication in PRL

Proton

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Day-to-day Variability Day-to-day Variability

Average Variability

Solar wind effects

Preliminary Data Please refer to the AMS forthcoming publication in PRL

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Forbush Decreases Forbush Decreases Identification Identification

Look for significant decreases in the daily proton flux, for each rigidity bin

2.97-3.29 GV 16.6-18.0 GV

Normalized Flux at 2.97–3.29 GV Normalized Flux at 16.6–18.0 GV

Preliminary Data, please refer to the AMS forthcoming publication in PRL Preliminary Data, please refer to the AMS forthcoming publication in PRL

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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Start date: date when decrease is first observed Date of minimum: date when majority of rigidity reach a minimum value Recovery date: date when normalized flux is within 2 SD of day-to-day variability Duration: number of days a decrease is observed Maximum rigidity: highest rigidity that shows a decrease Maximum decrease at 2 GV: percent decrease of the flux in the rigidity bin around 2 GV on the date of minimum.

FD Characteristics FD Characteristics

Preliminary Data Please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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FD events observed by AMS FD events observed by AMS

March 8, 2012

FD with long duration (20 days) and maximum decrease at 2 GV of 40%

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

Preliminary Data, please refer to the AMS forthcoming publication in PRL

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FD events observed by AMS FD events observed by AMS

August 6, 2011

FD with short duration (4 days) and maximum decrease at 2 GV of 15%

Preliminary Data, please refer to the AMS forthcoming publication in PRL

2.40-2.67 GV 3.29-3.64 GV 5.37-5.90 GV 10.1-11.0 GV 19.5-21.1 GV

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FD Event List FD Event List

List of FDs between May 2011 and May 2016 studied by AMS with estimated start date and duration.

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FD Relationship with Solar Wind FD Relationship with Solar Wind

AMS

SOLAR WIND

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Summary Summary

➢ AMS measures the daily proton flux with high

precision and resolution

➢ A method to identify decreases of the daily flux was

developed

➢ this method can be applied to heavier nuclei

➢ 33 Forbush decreases between May 2011 and May

2016 have been studied by AMS

➢ Time evolution in all rigidity bins is now

precisely measured →provides a deeper understanding of the short-term solar activity phenomena

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Thanks For Your Attention Thanks For Your Attention

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Backup Backup

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AMS Acquisition Rate AMS Acquisition Rate

Acquisition rate [Hz] Particle rates vary from 200 to 1600 Hz per orbit

In 6 years of operation, AMS has measured over 100 billion events.

Latitude Longitude Hz

The ISS orbits the Earth at 400 km altitude and 51.6° to the Equator.

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Distribution quiet period Distribution quiet period

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Mean of Distribution Mean of Distribution quite periods vs R quite periods vs R

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SD quite periods vs R SD quite periods vs R

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Correlations with ICMEs Correlations with ICMEs

The profile of a FD is influenced by the path through the interplanetary disturbances:

➢ The faster the propagation of the

interplanetary disturbance, the stronger its magnetic field, the faster the decrease

➢ The FD magnitude is larger for: ➢

Fast and wide ICME

➢

Stronger flares

➢

Source regions close to the center

  • f the solar disk

➢ FDs have generally smaller magnitude

when only the forward shock is present

➢ If ICME is preceded by a shock,

two-step pattern (1st shock, 2nd ejecta)

  • H. V.Cane, “Coronal Mass Ejections and Forbush Decreases”. Space Science Reviews, 93: 55-77, 2000
  • H. V. Cane et al., “Helios 1 and 2 observations of particle decreases, ejecta and magnetic cluds”. Journal of Geophysical Research, 99(A11)
  • A. Devos et al., “Geoeffectiveness of Coronal Mass Ejections in the SOHO era”, Solar Physics 290:579-612, 2015

Richardson, Cane, “Near-Earth Interplanetary Coronal Mass Ejections during Solar Cycle 23 (1996-2009): Catolog and Summary of Properties”

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Correlations with ICMEs Correlations with ICMEs

The profile of a FD is influenced by the path through the interplanetary disturbances:

➢ The faster the propagation of the

interplanetary disturbance, the stronger its magnetic field, the faster the decrease

➢ The FD magnitude is larger for: ➢

Fast and wide ICME

➢

Stronger flares

➢

Source regions close to the center

  • f the solar disk

➢ FDs have generally smaller magnitude

when only the forward shock is present

➢ If ICME is preceded by a shock,

two-step pattern (1st shock, 2nd ejecta)

  • H. V.Cane, “Coronal Mass Ejections and Forbush Decreases”. Space Science Reviews, 93: 55-77, 2000
  • H. V. Cane et al., “Helios 1 and 2 observations of particle decreases, ejecta and magnetic cluds”. Journal of Geophysical Research, 99(A11)
  • A. Devos et al., “Geoeffectiveness of Coronal Mass Ejections in the SOHO era”, Solar Physics 290:579-612, 2015

Richardson, Cane, “Near-Earth Interplanetary Coronal Mass Ejections during Solar Cycle 23 (1996-2009): Catolog and Summary of Properties”

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ICME & CIR ICME & CIR

ICMEs, CIRs and their shocks are responsible for the majority of Forbush decreases

Interplanetary Coronal Mass Ejections Corotating Interacting Regions

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AMS and Solar Wind AMS and Solar Wind

ICME events AMS WIND WIND WIND

Preliminary Data, please refer to the AMS forthcoming publication in PRL

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ICME in this time period AMS

AMS and Solar Wind AMS and Solar Wind

WIND WIND WIND

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CIR signature within this time period AMS

AMS and Solar Wind AMS and Solar Wind

WIND WIND WIND