PSP FIELDS Radio Frequency Spectrometer, RFS, High Frequency Receiver, HFR, Data:

The RFS is the high frequency component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1]. For a full description of the FIELDS experiment, see reference [2]. For a description of the RFS, see reference [3].

The RFS produces auto and cross spectral data products in two frequency ranges, the Low Frequency Reciever range and the High Frequency Receiver range. Telemetered spectral data products for both HFR and LFR contain 64 frequency bins, with the LFR typically covering a frequency range from 10.5 kHz to 1.7 MHz, and the HFR covering from 1.3 MHz to 19.2 MHz, with approximately logarithmically spaced bins. LFR high-resolution spectra contain 32 finely spaced frequency bins near the plasma frequency. The exact frequency bins are selectable and are included as metadata variables in this file.

The Level 2 data products contained in this data file have been calibrated for the preamp and RFS analog section response, the Polyphase Filter Bank, PFB, and the Fast Fourier Transform, FFT, spectral processing as described in reference [3]. Corrections for base capacitance and antenna effective length have not been applied. These corrections will be applied in Level 3 RFS data. Therefore, the units for all spectral quantities are given in V^2/Hz.

The time resolution of the RFS data vary with instrument mode. During encounter, which is when PSP is within 0.25 astronomical units, AU, of the Sun, the cadence for RFS HFR and LFR spectra is typically about 7 s. During cruise mode, which is the default mode for operations outside of 0.25 AU, the cadence for HFR and LFR spectra is about 56 s.

References:

• 1) Fox, N.J., Velli, M.C., Bale, S.D., et al., Space Sci Rev (2016), 204:7, DOI:10.1007/s11214-015-0211-6
• 2) Bale, S.D., Goetz, K., Harvey, P.R., et al., Space Sci Rev (2016), 204:49, DOI:10.1007/s11214-016-0244-5
• 3) Pulupa, M., Bale, S.D., Bonnell, J.W., et al., JGR Space Physics (2017), 122, 2836-2854, DOI:10.1002/2016JA023345

The data set contained in the ascii text files consist of the current sheet (CS) time intervals and the associated parameters of identified magnetic reconnection exhausts across CSs recorded by the Parker Solar Probe within R<0.26 AU from the Sun for close encounters 4-11. A detailed description is available in a manuscript submitted to The Astrophysical Journal by Eriksson et al. [2024] entitled "Parker Solar Probe Observations of Magnetic Reconnection Exhausts in Quiescent Plasmas Near the Sun". The ascii data file zenodo_psp_ce_lmn_cs_output_sorted_tctr.txt contains a center time of the optimized Walen relation (tc, column 1) and columns 2-3 show the CS start (CS1) and end (CS2) times. This is followed by the time duration dtcs in seconds (column 4) and whether a SPAN-I instrument survey (s=sf00) or burst (a=af00) data product exist (column 5). The RTN components of the adjacent time averaged magnetic field before (B1_R, B1_T, B1_N) and after (B2_R, B2_T, B2_N) the CS then follows in columns 6-11 and a corresponding magnetic field rotation angle (Bshear1) at the CS (column 12). The CP dL, dM, dN columns 13-15 list the distances covered along the hybrid-LMN coordinate system based in a Cross-Product normal to the CS in terms of the average ion inertial length diavg (column 16), which is based on a non-corrected proton density (Np1+Np2)/2=Npavg (columns 17-19). The subsequent columns 20-28 are the adjacent VL,VM,VN on the two sides of the CS from the MVAB LMN system as well as their averages (VL1+VL2)=VLavg, (VM1+VM2)/2=VMavg and (VN1+VN2)/2=VNavg. This is followed (columns 29-37) by the corresponding VL,VM,VN and averages in the hybrid-LMN system using the cross-product (CP) normal. The adjacent average total magnetic field Btot1 and Btot2 (columns 38-39) and the LMN components of the magnetic field in the MVAB system [BL1, BL2], [BM1, BM2], [BN1, BN2] in columns 40-45 are followed by the corresponding magnetic fields in the CP hybrid-LMN system (columns 46-51). The ratio of the intermediate to minimum eigenvalue ratio is included (column 52) followed by the unit vectors of the MVAB system L=[L_R, L_T, L_N], M=[M_R, M_T, M_N], and N=[N_R, N_T, N_N] in columns 53-61. The times adjacent to the CS used to obtain this set of MVAB eigenvectors is found in columns 62-63 (MVAB UT1 and MVAB UT2). The magnetic fields (B1 and B2) used to obtain the local hybrid-LMN system relative these MVAB times relatively farther from the CS are associated with a rotation angle (Bshear2) in column 64. The local hybrid-LMN system from the CP normal is then listed in columns 65-73 LCP=[L_R, L_T, L_N], MCP=[M_R, M_T, M_N], NCP=[N_R, N_T, N_N]. The angle (degrees) between the MVAB N and NCP is listed in column 74 (Nmv*Ncp) followed by the last two columns 75-76 that contain the time interval (s) relative CS1 and CS2 to obtain average plasma data (dext) and magentic field data (bext). A letter "m" right before column 1 flags the five events in this list of 236 events when the magnetic field did not change sign across the assumed CS. A letter "d" marks the 10 events associated with two opposite (double) exhausts. The ascii data file zenodo_psp_ce_lmn_cs_output_sorted_qtn.txt contains the same current sheet (CS) start (CS1) and end (CS2) times (columns 1-2). This file also lists the adjacent average proton (non-corrected) density in columns 3-4 as in the first (tctr) file which is followed by the average proton temperatures (Tp1 and Tp2 in columns 5-6), solar wind speed (Vtot1 and Vtot2 in columns 7-8) and the hybrid system L-components of the velocity (VL1 and VL2 in columns 9-10). Columns 11-16 contain the minimum and maximum values within each CS of the non-correct proton density, proton temperature and VL component. Column 17 lists the daily median density ratio from the electron density (Ne) and the non-corrected proton density (Np) where Ne is obtained through quasi-thermal noise spectroscopy by Kruparova et al. (2023). Column 18 lists the average of this daily ratio. Column 19 lists a value fc. A value larger than 1.0 indicates that a CS event time period is corrected to a local Ne value using Npfc=(Ne/Np)*Np*fc, where Np is a non-corrected proton density, Ne/Np is the median of the daily Ne/Np ratio. The ascii data file zenodo_psp_ce_lmn_cs_output_sorted_positions.txt contains the Parker Solar Probe median of its radial position within each CS1-CS2 time period in both solar radius and astronomical unit. The PDF figures psp_ceXX_apj_plots_qtn_final.pdf for XX=04,05,06,07,08,09,10 and 11 contain all CS events with a reconnection exhaust for each close encounter 04-11 on the basis of the agreement with a Walen prediction. Each plot shows the pitch-angle distribution (0-180 degrees) of the supra-thermal energy flux, proton temperature (MK), proton density (black) corrected to a daily median ratio Ne/Np as Npcorr=(Ne/Np)*Np, where Ne (red dots) is obtained from a QTN analysis by Kruparova et al. (2023), L-components of the magnetic field and proton velocity with a red trace showing a Walen prediction to this VL across the CS, the M and N components of the magnetic field with BM shifted by its time-period average, and the M and N components of the proton velocity with VM shifted by its time-period average. The LMN unit vectors of the employed hybrid LMN system are shown below each plot for reference. Finally, the eight ~11-day overview plots for each close encounter 4-11 marks the center times (tc) of each confirmed exhaust interval in this study of 231 events (red vertical dotted line) with the five marginal events marked as a black vertical dotted line. The panels from the top show the pitch-angle distribution (0-180 degrees) of the supra-thermal energy flux, proton temperature (MK), magnetic field strength, R-components of B and V, N-components of B and V, and the radial postion of Parker Solar Probe in terms of the solar radius. Here, R and N are two of the three RTN system components of B and V.

The SPDF Coordinated Heliospheric Observations Web, COHOWeb, hourly and daily Parker Solar Probe, PSP, data were made by using high resolution data from from CDAWeb.The PSP COHO file include data derived from the PSP FIELDS Fluxgate Magnetometer data as well as Densities, Vector Velocities, and Scalar Radial Component Temperatures of Solar Wind Protons measured by the PSP SWEAP Solar Probe Cup, SPC. The original PSP magnetic field data comes from the PSP_FLD_L2_MAG_RTN_1MIN data product while the original plasma data comes from the PSP_SWP_SPC_L3I data product by applying the following conditions: Proton bulk velocity from 1-dimensional Maxwellian fitting, only good quality, in the inertial RTN frame Total proton number density from 1-dimensional Maxwellian fitting, only good quality* Proton most probable thermal speed, radial component, from 1-dimensional maxwellian Fitting, only good qualityCitation: Papitashvili, N. E. (2020). Parker Solar Probe (PSP) Merged Magnetic Field, Plasma, and Ephemeris, Hourly Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/19ed-kz70

These are solar wind in situ data arrays in python pickle format suitable for machine learning, i.e. the arrays consist only of numbers, no strings and no datetime objects.See AAREADME_insitu_ML.txt for more explanation.If you use these data for peer reviewed scientific publications, please get in touch concerning usage and possible co-authorship by the authors (C. Möstl, A. J. Weiss, R. L. Bailey, R. Winslow, A. Isavnin, D. Stansby): christian.moestl@oeaw.ac.at or twitter @chrisoutofspace Made with https://github.com/cmoestl/heliocats Load in python with e.g. for Parker Solar Probe data:> import pickle> filepsp='psp_2018_2021_sceq_ndarray.p'> [psp,hpsp]=pickle.load(open(filepsp, "rb" ) ) plot time vs total field> import matplotlib.pyplot as plt> plt.plot(psp['time'],psp['bt'])Times psp[:,0 ] or psp['time'] are in matplotlib format. Variable 'hpsp' contains a header with the variable names and units for each column. Coordinate systems for magnetic field components are RTN (Ulysses), SCEQ (Parker Solar Probe, STEREO-A/B, VEX, MESSENGER), HEEQ (Wind)available parameters:bt = total magnetic fieldbxyz = magnetic field componentsvt = total proton speedvxyz = velocity components (only for PSP)np = proton densitytp = proton temperaturexyz = spacecraft position in HEEQr, lat, lon = spherical coordinates of position in HEEQ

The following datasets are the result of filtering algorithm applied to a wave analysis of Parker Solar Probe data from Encounters 8 to 16. The wave analysis was conducted by Kristoff Paulson using a Short-Time Fourier Transform (STFT) approach based on polarization techniques derived by Means, 1972 (DOI: 10.1029/JA077i028p055511135). Included is a jupyter notebook containing the filtering algorithm, the results of the filtering, and a demonstration of how to best open the files. The dataset for each encounter contains 9 columns that correspond with:

Date in CDF epoch

Left-handed (LH) Integrated Wave Power (nT^2) where integration is over frequency space (0-32 Hz) of filtered activity

Right-handed (RH) Integrated Wave Power (nT^2)

LH median ellipticity where median is over frequency space

RH median ellipticity

LH median coherency

RH median coherency

LH median wave normal angle (deg)

RH median wave normal angle (deg)

In all cases, ellipticity is measured in the Parker Solar Probe spacecraft frame. Ellipticity measures the ellipticity of the polarization ellipse and takes on values between -1 and 1. Values of 1 correspond with RH circular polarization and -1 with LH circular polarization. Coherency takes on values between 0 and 1. It measures how interrelated fluctuations are where 0 represents noise and 1 represents coherent fluctuations. The wave normal angle is the angle between the wave vector, k, and the local mean magnetic field, B. Since there are inherent ambiguities in the direction of the wave vector for single spacecraft measurements, the wave normal angle is calculated such that it takes on angles from 0 to 90 degrees. The filtering algorithm selects activity in which coherency is above 0.8, absolute value of ellipticity is above 0.5, and wave normal angle is below 45 degrees such that coherent, circularly polarized, near parallel propagating wave activity on ion scales is selected. If wave power for a given time has value of 0.0, then no fluctuations in the magnetic field data passed the required filters at that time.

:

The SPDF Coordinated Heliospheric Observations Web, COHOWeb, hourly and daily Parker Solar Probe, PSP, data were made by using high resolution data from from CDAWeb.The PSP COHO file include data derived from the PSP FIELDS Fluxgate Magnetometer data as well as Densities, Vector Velocities, and Scalar Radial Component Temperatures of Solar Wind Protons measured by the PSP SWEAP Solar Probe Cup, SPC. The original PSP magnetic field data comes from the PSP_FLD_L2_MAG_RTN_1MIN data product while the original plasma data comes from the PSP_SWP_SPC_L3I data product by applying the following conditions:* Proton bulk velocity from 1-dimensional Maxwellian fitting, only good quality, in the inertial RTN frame* Total proton number density from 1-dimensional Maxwellian fitting, only good quality* Proton most probable thermal speed, radial component, from 1-dimensional maxwellian Fitting, only good qualityCitation: Papitashvili, N. E. (2020). Parker Solar Probe (PSP) Merged Magnetic Field, Plasma, and Ephemeris, Hourly Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/19ed-kz70

Heliocentric trajectories for Parker Solar Probe in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, CoordinatesThe original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth.The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch" which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage:+---------------------------------------------------------------------+| Method Name | FPA Longitude Definition ||---------------------------------------------------------------------|| B1950.0 | the actual FPA at 22:09 UT on December 31, 1949 || J2000.0 | the smoothed FPA at 12:00 UT on January 1, 2000 || True of Date | the actual FPA at 00:00 UT on the date of interest || Mean of Date | the smoothed FPA at 00:00 UT on the date of interest |+---------------------------------------------------------------------+The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method.More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.Citation: Szabo, A. (2020). Parker Solar Probe Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/41s1-hx58

Parker Solar Probe kısaltılmış PSP daha önce Solar Probe Solar Probe Plus veya Solar Probe Güneş in dış koronasını gözle

Mpeg movies created using the L3 data product. These data are separated by encounter and by camera ("inner" and "outer")

Heliocentric trajectories for Parker Solar Probe in Heliographic, HG, Heliographic Inertial, HGI, and Solar Ecliptic, SE, CoordinatesThe original trajectory data are taken from http://ssd.jpl.nasa.gov/horizons.cgi where users can find many more objects. In the case of orbit data for planets, the orbit data can be used as a proxy for spacecraft ephemeris that are in orbit about the planets. On a heliospheric scale, differences between the planet orbital tarjectory and that of the spacecraft are very small. For instance, the heliocentric longitudes differ by only 0.25° for a spacecraft stationed near the L1 Lagrange point at approximately 100 Earth radii upstream of the Earth.The production of the HG, HGI, and SE trajectory data requires a values for the "Equinox Epoch" which is defined as the epoch time when the direction from the Earth to the sun at the time of the vernal equinox when the sun seems to cross equatorial plane of the Earth from below. This direction is called the First Point of Aries, FPA and it is not a fixed direction but drifts by about 1.4° per century or 50.26" per year. In addition, there are tiny irregularities in FPA drift that are on the order of 1" per year or less. The Equinox Epoch can be determined by using a variety of methods for calculating the instantaneous FPA longitudinal direction and whether the tiny irregularities have been smoothed or averaged out. Four methods for determining the Equinox Epoch are in common usage:+---------------------------------------------------------------------+| Method Name | FPA Longitude Definition ||---------------------------------------------------------------------|| B1950.0 | the actual FPA at 22:09 UT on December 31, 1949 || J2000.0 | the smoothed FPA at 12:00 UT on January 1, 2000 || True of Date | the actual FPA at 00:00 UT on the date of interest || Mean of Date | the smoothed FPA at 00:00 UT on the date of interest |+---------------------------------------------------------------------+The heliocentric trajectory data included in this data product have been calculated by using the Equinox Epoch: defined via the "Mean of Date" method.More precise coordinates, and some planet-centered coordinates, are found in the "traj" subdirectories of spacecraft specific directories at https://spdf.gsfc.nasa.gov/pub/data/ and http://ssd.jpl.nasa.gov/horizons.cgi.Citation: Szabo, A. (2020). Parker Solar Probe Ephemeris, Heliocentric Trajectories, Heliographic, Heliographic Inertial, and Solar Ecliptic Coordinates, HelioWeb, Daily Data [Data set]. NASA Space Physics Data Facility. https://doi.org/10.48322/41s1-hx58

This is the HELIO4CAST lineup vcatalog, for multipoint observations of interplanetary coronal mass ejection (ICME). This is version 3.0, released 2025-April-25, updated 2025-April-25.The catalog is published at https://helioforecast.space/lineupsRules: If this catalog is used for results that are published in peer-reviewed international journals, please contact chris.moestl@outlook.com, eva.weiler@geosphere.at and emma.davies@geosphere.at for possible co-authorships.An initial catalog version was presented in Möstl et al. (2022) ApJLetters, https://iopscience.iop.org/article/10.3847/2041-8213/ac42d0

Reproduction data for two figures (4 and 6) which were produced for the review paper 'Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter'. Other figures are previously published. The work presents a review of dust measurements from spacecraft Cassini, STEREO, MMS, Cluster, Maven and WIND. We also consider the details of dust impacts and charge generation, and how different antenna signals can be generated. We compare observational data to laboratory experiments and simulations and discuss the consequences for dust observation with the new NASA Parker Solar Probe and ESA Solar Orbiter spacecraft. 'Figure 4' has formats TXT and CSV, and each file is name according to which panel (and bias) it represents. The files are two dimensional an the first column is time in microseconds before impact event, and the second column is recorded voltage. 'Figure 6' is in CDF (common data format) format. A suitable software must be used to handle the data (See NASA documentation for CDF format v 3.7.1: https://cdf.gsfc.nasa.gov/html/FAQ.html). 'mms1_edp_BURST_SC-POTENTIAL_2016-11.cdf' contains data for panel 3, SC potential. 'mms1_edp_BURST_DC_2016-11.cdf' contains monopole and dipole data. Both these sets are for burst mode operation.

These are the figures I have used for the manuscript entitled'Time Profile Study of Type III Solar Radio Bursts using Parker Solar Probe".

Supplementary data to "Diverse dust populations in the near-Sun environment characterized by PSP/ISʘIS."

The ISʘIS data and visualization tools are available to the community at https://spacephysics.princeton.edu/missions-instruments/PSP; data are also available via the NASA Space Physics Data Facility (https://spdf.gsfc.nasa.gov/) and ISʘIS science operation center (SOC, https://spp-isois.sr.unh.edu/home.html). The FIELDS data are available at https://fields.ssl.berkeley.edu/data/.

This poster was shown at EGU 2019.

The FIELDS instrument combines magnetic and electric field measurements into a single, coordinated experiment. Magnetic fields are measured using both fluxgate and search-coil induction magnetometers mounted on a deployable boom in the spacecraft umbra. FIELDS will make electric field measurements both as a current-biased, resistively-coupled, double-probe instrument (Harvey et al. 1995, Bonnell et al. 2009, Wygant et al. 2013) and as a capacitively-coupled radio and plasma wave instrument (Bougeret et al. 1995, 2008). The V1, V2, V3, and V4 electric field probes are mounted at the base of the Parker Solar Probe, PSP, Thermal Protection System, TPS, or heat shield and deploy out into full sunlight. At the PSP perihelion altitude of 9.8 solar radii, these antennas will reach temperatures of more than 1300°C. Another simple voltage sensor, the V5 antenna, is mounted on the magnetometer boom in the umbra of the spacecraft.

These are solar wind in situ data arrays in python pickle format suitable for creating catalogs, plots and movies of interplanetary coronal mass ejections (ICME). They are used to calculate parameters in this ICME catalog:https://helioforecast.space/icmecatIf you use these data for peer reviewed scientific publications, please get in touch via chris.moestl@outlook.com concerning usage and possible co-authorship.Made with https://github.com/cmoestl/heliocats

ග න ව ග න ඉත හ සය ග න භ ව තය ග ල ය ග න භ ව තය ප රදත තම ම ප රදස න හ ව ශ ලත වය 600 600 ප ක සල අන ක ත ව භ දනයන 240 240 ප ක

This is the HELCATS interplanetary coronal mass ejection (ICME) catalog, based on in situ magnetic field and bulk plasma observations in the heliosphere. This is version 2.0, released 2020-06-03, updated 2020-06-12also available at: https://helioforecast.space/icmecatThe catalog is available as python pandas dataframe (pickle), python numpy structured array (pickle), json, csv, xlsx, txt, hdf5, html, plus a header txt file with parameter descriptions. Number of events in ICMECAT: 739ICME observatories: Parker Solar Probe (PSP), Wind, MAVEN, STEREO-A, STEREO-B, Venus Express (VEX), MESSENGER, Ulysses.Time range: January 2007 - December 2019.Authors: Christian Möstl, Andreas J. Weiss, Rachel L. Bailey, Martin A. Reiss, Space Research Institute (IWF), Austrian Academy of Sciences, Graz, Austria. Contributors: Peter Boakes, Alexey Isavnin, Emilia Kilpua, David Stansby, Reka Winslow, Brian Anderson, Lydia Philpott, Vratislav Krupar, Jonathan Eastwood, Simon Good, Lan Jian, Teresa Nieves-Chinchilla, Cyril Simon Wedlund, Jingnan Guo, Mateja Dumbovic, Johan von Forstner, Benoit Lavraud. Rules: If results are produced with this catalog for peer-reviewed scientific publications, please contact christian.moestl@oeaw.ac.at for possible co-authorship.

The steady state solar wind ambient is obtained with three dimensional magnetohydrodynamics (MHD) numerical model. To verify the capability of the model in producing structured solar wind, the modeled datas are compared with Parker Solar Probe (PSP) in situ observations during its first two encounters, as well as Wind observations at 1AU.