when you must make changes to (pre)approved data groups in
TRANSCRIPT
Presentation Title Should not exceed two lines Try to avoid changes
within T-6 where possible.
If you need to make a change (inside of T-6 weeks, after the proxy pulse shape is pre- approved, after the final pulse shape is approved), follow this process — Email the expert groups ([email protected]) before you withdraw the
shot stating • The experiment ID and shot date (on the subject line of the email would be best) • Who is requesting the change (i.e. RI, expert group, etc…) • What the change is and why the request for the change (i.e. wavelength change for
facility convenience) • Who is making the change (i.e. RI, BLIP, etc…) • When the changes are expected to be complete and the data group resubmitted.
If you must make a change and you know you will, don’t sign off on RI final pulse-shape approval until the change is implemented. — Each time you sign off the approval the expert groups start the review cycle over again.
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
[email protected]
mailto:[email protected]
LLNL-PRES-729670
2
Between T-6 weeks and T-3 weeks, Expert Groups are making assessments based on submitted materials (TaLIS viewgraphs, pre-approved pulse shape, etc.). — Changes at this time can come from the RI/shot team or from the Expert Groups — The purpose of the email is to socialize an “update” to submitted materials and guide the
assessment process.
Between T-3 weeks (the set-up review) and the NOM final approval, requests for changes come from Expert Group guidance (your TAS jaw positions are wrong, your beam energies are above filamentation thresholds, etc.) — Changes in this window should not come from programmatic considerations — The RI for a particular shot should still use this email as a method to capture what is changed, and
what approval was dropped so that Expert Group reviewers (i) know that their request has been carried out, and (ii) when parasitic groups are affected, they know what level of re-assessment is required.
The process is roughly analogous to a change of Shot Planner data via an SCR, where the approve/reject function in AppMan replaces the approve/reject in the SCR. — The process is not perfect: the SCRs are better archived, and display information/status visually in
a graphical way. Communication among people on the listserv emails is “broken” by one person choosing not to “reply all”.
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
Note the expert groups do not make any changes to a setup themselves, it is the RI’s responsibility to make and notify all of those changes.
LLNL-PRES-729670 3
For target shots that are expected to produce unclassified data from the SuperSnout-II run in secure mode
The RI must initiate the process in AppMan and by contacting Kevin directly.
1. The Shot RI makes an annotation in AppMan requesting special review of film on SuperSnout-II for possible unclassified determination. In addition, the RI should contact Kevin Fournier at that time to confirm he can support the review. [This only applies to the film from SS-II, for now.] • Example: INFO: Central channel SS-II imaging data are expected to be unclassified. We are
requesting an appropriate DC review of the film post-shot to determine its status.
2. If KF agrees, he will annotate in the classification review tracker that it is OK to review the SS-II film post-shot and make a determination then.
3. If KF has approved, when Tom Kohut reviews the shot, Tom updates the classification annotations to direct the photolab team how to proceed (this will include use of the new form that Bob Ehrlich worked out with OCEC). • Classified Film & IP processing in photolab per NIF-5055393. For this shot, the PDIM
SSII film data may be verified by a DC to not contain classified spectral data. When called out in the procedure, contact Kevin Fournier to review film prior to final marking. He will review the data and communicate to me the result.
LLNL-PRES-729670 4
Need help? Need help finding help?
Don’t hesitate to contact the User Office, we’re here to help!
Contact the NIF User Office: [email protected]
We also maintain a list of points of contact for all systems at NIF: https://lasers.llnl.gov/content/assets/docs/for-users/nif-point-of- contacts.pdf
We also maintain a list of diagnostic SM & RS points of contact: https://lasers.llnl.gov/content/assets/docs/for-users/diagnostic-RS- contact-list.xlsx
We have published a 2016 update to the NIF User Guide: https://lasers.llnl.gov/content/assets/docs/for-users/2016-user- guide.pdf
Status of NEPPS (NIF Electron-Positron-Proton Spectrometer)
Hui Chen With input from D. Kalantar, H-S Park, T. Ma, Mike Rosenberg, H. Rinderknecht and N.
Thompson
1. Physics background
4. New development – NEPPS-300G & - 9kG
7
High energy (keV - MeV) electrons, positron and ions can be produced from laser plasma interactions
e+ e+
e+ e+
8
The distribution of these particles is sensitive to the laser & target parameters
~1 MeV
Electron spectrum at 1015 W/cm2 Electron spectra at 1019 W/cm2
9
• Relativistic pair plasma: 1 – 20 MeV electrons/positrons
• Proton acceleration & heating: 0.1 – >10 MeV protons
• Magnetic reconnection: 0.01 – 0.1 MeV electrons
• Electron acceleration through collisionless shock:
0.5 – 5 MeV protons
10
Example: EPPS results at various laser energies provide data for the scaling study in the NIF pair plasma DS project
ARC
1st generation: Scintillating fiber & CCD based spectrometers
Engineers: Barry, Booth, Bruns
Target wheel
FACES
Dual system: Image plates provided additional measure of energy spectra for both positrons and electrons.
Sample Spectra: Fiber
Energy (keV)
The energy resolution for the electrons is 50 times higher with image plates.
Sample Spectrum: Image Plate
Engineers: Barry, Bruns
13
Fiber based
Image-plate based
Chen et al. Review of Scientific Instruments, (2003).
Thanks to Harry McLean et al.
15
Chen et al., Review of Scientific Instruments, (2008).
Y. Ping’s
2 keV - 1 MeV
0.1 MeV - 4 MeV
0.1 MeV - 4 MeV
0.8 MeV - 100 MeV
1 MeV - 6 MeV
10 KeV - 0.8 MeV
Tight Focus
1E8
1E7
1000000
100000
10000
5
4
3
2
1
0
17
EPPS is now available on OMEGA EP, ORION and LFEX laser facilities
EPPS on GEKKO LFEX chamber
EPPS Mounting Frame
Engineer: Shannon Ayers Engineers: Bruns & team Students: Jaebum Park, Jackson Williams
18
Three NIF EPPS have been built using the same design
Half Section View of the NEPPS Assembly
TCC
Energy Coverage
Tunable spectral window within the 800 keV to 100 MeV electron energy range
Resolving Power ≥ E /E ~ 1-100
Data Collection Image Plates
RE: Shannon Ayers
RCF film pack
Calibration was inferred from prior experiments and field strength measurements.
19
NEPPS is operational: it has been used in three NIF ARC shots
Electron spectrum Proton spectrum N160324-001-999
(Shot RI: D. Martinez)
ARC Relativistic Pair Plasma Experiment Layout - Target Chamber (Top View)
NEPPS will be the primary diagnostic on the NIF pair plasma DS shots in May 2017 and Proton heating DS shot in 2018
(90,0)
NEPPS
NEPPS
ARC-driven TNSA protons will be characterized and used for isochoric
heating of mid-Z materials
Proton Acceleration and Heating with NIF ARC
PI: T. Ma, D. Mariscal, C. McGuffeyPI: H. Chen, G. J. Williams
21
Electrons are accelerated by the reconnection electric field, being injected at varied distances from the X points and trapped in plasmoids
Physics for the new NEPPS: We are studying astrophysical particle acceleration via three different physics mechanisms
Totorica et al. PRL 116, 095003 (2016)
Magnetic Reconnection (MagRecon team)
Second-order Fermi acceleration
Electron spectrum
Particles gain energy traveling through shock wave repeatedly reflected by a moving changes in the magnetic field
Particles gain energy during the motion of a charged particle in the presence of randomly moving magnetic mirrors
PIC simulation by A. Spitkovsky
Magnetic filaments
Particle energy
Small scale dynamo can amplify the seed magnetic fields
NIF experiment will attempt to measure proton spectrum change going through turbulent magnetic fields
FLASH simulation by P. Tzeferacos
Particle acceleration in shocks: first order in v/c and scatters off moving magnetic fields
Magnetic filaments
Particle energy
Non-thermal energy gain
PI: W. Fox PI: Y. Sakawa & F. Fiuza PI: G. Gregori
22
Particles Parameter NEPPS NEPPS-B300G Electron matters
NEPPS-B9kG Proton matters
Electrons Energy range 0.1 – 100 MeV 0-200 keV -
Energy resolution 100 keV <10% depending on slit and pinhole sizes -
Protons Energy range 1-100 MeV - 0.5 – 5 MeV
Energy resolution - 8% with 0.5 mm slit
Item NEPPS NEPPS-B300G Electron matters
NEPPS-B9kG Proton matters
# of units 3 2 1
Line-of sight Only Equatorial DIMS Only Equatorial DIMS (as of May/17) Only Equatorial DIMS (as of May/17)
Detector Image plate Image plate Image plate
Detector Filtering Not possible Not possible for May 2017 Not possible for May 2017
Mag Field strength ~0.8 T 0.03T >0.9T
First experiment 2016 May, 2017 May 2017
23
NEPPS-B300G is modified version of the NEPPS to detect low energy electrons at higher resolution
Image plate
Front cover Replaceable slit or pinholes
Existing NEPPS electron tracking is 0.1 to 80 MeV with B field = 0.8T
NEPPS-B300G electron tracking is 2-2000 keV with B field = 0.03T
Electron tracing: G. Fiksel
24
NEPPS-B9kG are using high-field magnet to deflect 0.5 to 4 MeV protons with ~8% energy resolution
1
e- detectorp+ detector
0.5 mmSlit aperture: Resolution is set by an adjustable aperture: 0.5 mm E/E = 8%
B = -1.0 Tesla
Single Magnets, multiple configurations
Flexible Configurability Improved Slit/IP Alignment Improved B Field Uniformity
Existing NEPPS:
New NEPPS:
26
Drawings, Bids, Fab order out – Feb 2017
Assembly and Testing – April 2017
First NIF experiment – May 15th week of 2017 for ACSEL and MagRecon campaigns
Schedule and availability of NEPPS-B300G and NEPPS-B9kG
27
NEPPS • Relativistic pair plasma: 1 – 20 MeV electrons/positrons
• Proton acceleration & heating: 0.1 – ~10 MeV protons
NEPPS-B300G & NEPPS-B9kG • Magnetic reconnection: 0.01 – 0.1 MeV electrons
• ACSEL
• ..
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
For target shots that are expected to produce unclassified data from the SuperSnout-II run in secure mode
Need help? Need help finding help?
Status of NEPPS (NIF Electron-Positron-Proton Spectrometer)
NIF-EPPS is an passive magnetic Electron-Positron-Proton Spectrometer to measure MeV particles
High energy (keV - MeV) electrons, positron and ions can be produced from laser plasma interactions
The distribution of these particles is sensitive to the laser & target parameters
Different project focus on different particle & energy coverage
Example: EPPS results at various laser energies provide data for the scaling study in the NIF pair plasma DS project
1st generation: Scintillating fiber & CCD based spectrometers
2nd generation: Scintillating fiber & Image plate spectrometer
3rd generation: image-plate based electron-positron-proton spectrometer (EPPS)
Calibration- scintillating fiber & CCD based spectrometer
Response calibration for Image plate based spectrometer
Quantitative overlaps were achieved among different electron spectrometers for various energy range
EPPS is now available on OMEGA EP, ORION and LFEX laser facilities
Three NIF EPPS have been built using the same design
NEPPS is operational: it has been used in three NIF ARC shots
NEPPS will be the primary diagnostic on the NIF pair plasma DS shots in May 2017 and Proton heating DS shot in 2018
Physics for the new NEPPS: We are studying astrophysical particle acceleration via three different physics mechanisms
Different NEPPS covers different parameters
NEPPS-B300G is modified version of the NEPPS to detect low energy electrons at higher resolution
NEPPS-B9kG are using high-field magnet to deflect 0.5 to 4 MeV protons with ~8% energy resolution
Changes over existing NEPPS design
Schedule and availability of NEPPS-B300G and NEPPS-B9kG
Multiple configuration of NEPPS will be available for NIF
Slide Number 28
If you need to make a change (inside of T-6 weeks, after the proxy pulse shape is pre- approved, after the final pulse shape is approved), follow this process — Email the expert groups ([email protected]) before you withdraw the
shot stating • The experiment ID and shot date (on the subject line of the email would be best) • Who is requesting the change (i.e. RI, expert group, etc…) • What the change is and why the request for the change (i.e. wavelength change for
facility convenience) • Who is making the change (i.e. RI, BLIP, etc…) • When the changes are expected to be complete and the data group resubmitted.
If you must make a change and you know you will, don’t sign off on RI final pulse-shape approval until the change is implemented. — Each time you sign off the approval the expert groups start the review cycle over again.
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
[email protected]
mailto:[email protected]
LLNL-PRES-729670
2
Between T-6 weeks and T-3 weeks, Expert Groups are making assessments based on submitted materials (TaLIS viewgraphs, pre-approved pulse shape, etc.). — Changes at this time can come from the RI/shot team or from the Expert Groups — The purpose of the email is to socialize an “update” to submitted materials and guide the
assessment process.
Between T-3 weeks (the set-up review) and the NOM final approval, requests for changes come from Expert Group guidance (your TAS jaw positions are wrong, your beam energies are above filamentation thresholds, etc.) — Changes in this window should not come from programmatic considerations — The RI for a particular shot should still use this email as a method to capture what is changed, and
what approval was dropped so that Expert Group reviewers (i) know that their request has been carried out, and (ii) when parasitic groups are affected, they know what level of re-assessment is required.
The process is roughly analogous to a change of Shot Planner data via an SCR, where the approve/reject function in AppMan replaces the approve/reject in the SCR. — The process is not perfect: the SCRs are better archived, and display information/status visually in
a graphical way. Communication among people on the listserv emails is “broken” by one person choosing not to “reply all”.
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
Note the expert groups do not make any changes to a setup themselves, it is the RI’s responsibility to make and notify all of those changes.
LLNL-PRES-729670 3
For target shots that are expected to produce unclassified data from the SuperSnout-II run in secure mode
The RI must initiate the process in AppMan and by contacting Kevin directly.
1. The Shot RI makes an annotation in AppMan requesting special review of film on SuperSnout-II for possible unclassified determination. In addition, the RI should contact Kevin Fournier at that time to confirm he can support the review. [This only applies to the film from SS-II, for now.] • Example: INFO: Central channel SS-II imaging data are expected to be unclassified. We are
requesting an appropriate DC review of the film post-shot to determine its status.
2. If KF agrees, he will annotate in the classification review tracker that it is OK to review the SS-II film post-shot and make a determination then.
3. If KF has approved, when Tom Kohut reviews the shot, Tom updates the classification annotations to direct the photolab team how to proceed (this will include use of the new form that Bob Ehrlich worked out with OCEC). • Classified Film & IP processing in photolab per NIF-5055393. For this shot, the PDIM
SSII film data may be verified by a DC to not contain classified spectral data. When called out in the procedure, contact Kevin Fournier to review film prior to final marking. He will review the data and communicate to me the result.
LLNL-PRES-729670 4
Need help? Need help finding help?
Don’t hesitate to contact the User Office, we’re here to help!
Contact the NIF User Office: [email protected]
We also maintain a list of points of contact for all systems at NIF: https://lasers.llnl.gov/content/assets/docs/for-users/nif-point-of- contacts.pdf
We also maintain a list of diagnostic SM & RS points of contact: https://lasers.llnl.gov/content/assets/docs/for-users/diagnostic-RS- contact-list.xlsx
We have published a 2016 update to the NIF User Guide: https://lasers.llnl.gov/content/assets/docs/for-users/2016-user- guide.pdf
Status of NEPPS (NIF Electron-Positron-Proton Spectrometer)
Hui Chen With input from D. Kalantar, H-S Park, T. Ma, Mike Rosenberg, H. Rinderknecht and N.
Thompson
1. Physics background
4. New development – NEPPS-300G & - 9kG
7
High energy (keV - MeV) electrons, positron and ions can be produced from laser plasma interactions
e+ e+
e+ e+
8
The distribution of these particles is sensitive to the laser & target parameters
~1 MeV
Electron spectrum at 1015 W/cm2 Electron spectra at 1019 W/cm2
9
• Relativistic pair plasma: 1 – 20 MeV electrons/positrons
• Proton acceleration & heating: 0.1 – >10 MeV protons
• Magnetic reconnection: 0.01 – 0.1 MeV electrons
• Electron acceleration through collisionless shock:
0.5 – 5 MeV protons
10
Example: EPPS results at various laser energies provide data for the scaling study in the NIF pair plasma DS project
ARC
1st generation: Scintillating fiber & CCD based spectrometers
Engineers: Barry, Booth, Bruns
Target wheel
FACES
Dual system: Image plates provided additional measure of energy spectra for both positrons and electrons.
Sample Spectra: Fiber
Energy (keV)
The energy resolution for the electrons is 50 times higher with image plates.
Sample Spectrum: Image Plate
Engineers: Barry, Bruns
13
Fiber based
Image-plate based
Chen et al. Review of Scientific Instruments, (2003).
Thanks to Harry McLean et al.
15
Chen et al., Review of Scientific Instruments, (2008).
Y. Ping’s
2 keV - 1 MeV
0.1 MeV - 4 MeV
0.1 MeV - 4 MeV
0.8 MeV - 100 MeV
1 MeV - 6 MeV
10 KeV - 0.8 MeV
Tight Focus
1E8
1E7
1000000
100000
10000
5
4
3
2
1
0
17
EPPS is now available on OMEGA EP, ORION and LFEX laser facilities
EPPS on GEKKO LFEX chamber
EPPS Mounting Frame
Engineer: Shannon Ayers Engineers: Bruns & team Students: Jaebum Park, Jackson Williams
18
Three NIF EPPS have been built using the same design
Half Section View of the NEPPS Assembly
TCC
Energy Coverage
Tunable spectral window within the 800 keV to 100 MeV electron energy range
Resolving Power ≥ E /E ~ 1-100
Data Collection Image Plates
RE: Shannon Ayers
RCF film pack
Calibration was inferred from prior experiments and field strength measurements.
19
NEPPS is operational: it has been used in three NIF ARC shots
Electron spectrum Proton spectrum N160324-001-999
(Shot RI: D. Martinez)
ARC Relativistic Pair Plasma Experiment Layout - Target Chamber (Top View)
NEPPS will be the primary diagnostic on the NIF pair plasma DS shots in May 2017 and Proton heating DS shot in 2018
(90,0)
NEPPS
NEPPS
ARC-driven TNSA protons will be characterized and used for isochoric
heating of mid-Z materials
Proton Acceleration and Heating with NIF ARC
PI: T. Ma, D. Mariscal, C. McGuffeyPI: H. Chen, G. J. Williams
21
Electrons are accelerated by the reconnection electric field, being injected at varied distances from the X points and trapped in plasmoids
Physics for the new NEPPS: We are studying astrophysical particle acceleration via three different physics mechanisms
Totorica et al. PRL 116, 095003 (2016)
Magnetic Reconnection (MagRecon team)
Second-order Fermi acceleration
Electron spectrum
Particles gain energy traveling through shock wave repeatedly reflected by a moving changes in the magnetic field
Particles gain energy during the motion of a charged particle in the presence of randomly moving magnetic mirrors
PIC simulation by A. Spitkovsky
Magnetic filaments
Particle energy
Small scale dynamo can amplify the seed magnetic fields
NIF experiment will attempt to measure proton spectrum change going through turbulent magnetic fields
FLASH simulation by P. Tzeferacos
Particle acceleration in shocks: first order in v/c and scatters off moving magnetic fields
Magnetic filaments
Particle energy
Non-thermal energy gain
PI: W. Fox PI: Y. Sakawa & F. Fiuza PI: G. Gregori
22
Particles Parameter NEPPS NEPPS-B300G Electron matters
NEPPS-B9kG Proton matters
Electrons Energy range 0.1 – 100 MeV 0-200 keV -
Energy resolution 100 keV <10% depending on slit and pinhole sizes -
Protons Energy range 1-100 MeV - 0.5 – 5 MeV
Energy resolution - 8% with 0.5 mm slit
Item NEPPS NEPPS-B300G Electron matters
NEPPS-B9kG Proton matters
# of units 3 2 1
Line-of sight Only Equatorial DIMS Only Equatorial DIMS (as of May/17) Only Equatorial DIMS (as of May/17)
Detector Image plate Image plate Image plate
Detector Filtering Not possible Not possible for May 2017 Not possible for May 2017
Mag Field strength ~0.8 T 0.03T >0.9T
First experiment 2016 May, 2017 May 2017
23
NEPPS-B300G is modified version of the NEPPS to detect low energy electrons at higher resolution
Image plate
Front cover Replaceable slit or pinholes
Existing NEPPS electron tracking is 0.1 to 80 MeV with B field = 0.8T
NEPPS-B300G electron tracking is 2-2000 keV with B field = 0.03T
Electron tracing: G. Fiksel
24
NEPPS-B9kG are using high-field magnet to deflect 0.5 to 4 MeV protons with ~8% energy resolution
1
e- detectorp+ detector
0.5 mmSlit aperture: Resolution is set by an adjustable aperture: 0.5 mm E/E = 8%
B = -1.0 Tesla
Single Magnets, multiple configurations
Flexible Configurability Improved Slit/IP Alignment Improved B Field Uniformity
Existing NEPPS:
New NEPPS:
26
Drawings, Bids, Fab order out – Feb 2017
Assembly and Testing – April 2017
First NIF experiment – May 15th week of 2017 for ACSEL and MagRecon campaigns
Schedule and availability of NEPPS-B300G and NEPPS-B9kG
27
NEPPS • Relativistic pair plasma: 1 – 20 MeV electrons/positrons
• Proton acceleration & heating: 0.1 – ~10 MeV protons
NEPPS-B300G & NEPPS-B9kG • Magnetic reconnection: 0.01 – 0.1 MeV electrons
• ACSEL
• ..
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
When you must make changes to (pre)approved data groups in your shot set ups inside T-6 weeks
For target shots that are expected to produce unclassified data from the SuperSnout-II run in secure mode
Need help? Need help finding help?
Status of NEPPS (NIF Electron-Positron-Proton Spectrometer)
NIF-EPPS is an passive magnetic Electron-Positron-Proton Spectrometer to measure MeV particles
High energy (keV - MeV) electrons, positron and ions can be produced from laser plasma interactions
The distribution of these particles is sensitive to the laser & target parameters
Different project focus on different particle & energy coverage
Example: EPPS results at various laser energies provide data for the scaling study in the NIF pair plasma DS project
1st generation: Scintillating fiber & CCD based spectrometers
2nd generation: Scintillating fiber & Image plate spectrometer
3rd generation: image-plate based electron-positron-proton spectrometer (EPPS)
Calibration- scintillating fiber & CCD based spectrometer
Response calibration for Image plate based spectrometer
Quantitative overlaps were achieved among different electron spectrometers for various energy range
EPPS is now available on OMEGA EP, ORION and LFEX laser facilities
Three NIF EPPS have been built using the same design
NEPPS is operational: it has been used in three NIF ARC shots
NEPPS will be the primary diagnostic on the NIF pair plasma DS shots in May 2017 and Proton heating DS shot in 2018
Physics for the new NEPPS: We are studying astrophysical particle acceleration via three different physics mechanisms
Different NEPPS covers different parameters
NEPPS-B300G is modified version of the NEPPS to detect low energy electrons at higher resolution
NEPPS-B9kG are using high-field magnet to deflect 0.5 to 4 MeV protons with ~8% energy resolution
Changes over existing NEPPS design
Schedule and availability of NEPPS-B300G and NEPPS-B9kG
Multiple configuration of NEPPS will be available for NIF
Slide Number 28