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21 results for “Bow shock”

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zenodo48/100

Predicted times of bow Shock crossings at Venus from the ESA/Venus Express mission, using spacecraft ephemerides and magnetic field data, with a predictor-corrector algorithm

CHARACTERISTICS Planet: Venus Radius: RV = 6051.8 km (volumetric mean planetary radius) Spacecraft: ESA/Venus Express Spacecraft coordinates system: Venus Solar Orbital (VSO) equivalent to Sun-State coordinate system: <ul> <li>+XVSO points towards the Sun from the planet’s centre,</li> <li>+ZVSO towards Venus’ North pole and perpendicular to the orbital plane defined as the XVSO–YVSO plane passing through the centre of Venus,</li> <li>YVSO completes the orthogonal system.</li> </ul> Time span: 01/04/2006 to 25/11/2014 Total number N of candidate bow shock crossings in the database: N = 4950 Number of quasi-parallel bow shock crossings: N|| = 844 Number of quasi-perpendicular bow shock crossings: N\(\perp\) = 4106 ORIGINAL DATASETS USED The original Venus Express/MAG data repository on which these algorithms were applied is available on ESA's Planetary Science Archive system (PSA) at: https://archives.esac.esa.int/psa/ftp/VENUS-EXPRESS/MAG/. For this study, 1-Hz magnetic field data was used. METHOD To construct this database from the original datasets above, the predictor and predictor-corrector algorithms used are described for the Mars case in: Simon Wedlund, C., Volwerk, M., Beth, A., Mazelle, C., Möstl, C., Halekas, J., Gruesbeck, J. and Rojas-Castillo, D., (2021), A Fast Bow Shock Location Predictor-Estimator From 2D and 3D Analytical Models: Application to Mars and the MAVEN mission, Journal of Geophysical Research, 127, e2021JA029942. <a href="https://doi.org/10.1029/2021JA029942">https://doi.org/10.1029/2021JA029942</a> They consist of two consecutive steps:  <ol> <li>Predictor geometric algorithm based on 2D or 3D existing fits for prediction of the Venus bow shock position. The original fits were taken from 2D conic fits in the plane \(\left(X_\text{VSO}, \sqrt{Y_\text{VSO}^2+Z_\text{VSO}^2}\right)\)performed on the datasets of Persson et al. (2023), Venusian bow shock crossings manually identified from measurements by the ASPERA-4 and MAG instruments onboard Venus Express, Zenodo (<a href="http://doi.org/10.5281/zenodo.7679677">https://doi.org/10.5281/zenodo.7679677</a>).</li> <li>Corrector algorithm based on magnetic field measurements.</li> </ol> We also provide the angle between the average Interplanetary Magnetic Field (IMF) vector upstream of the shock and the shock normal, noted θBn (ThetaBn). Assuming a locally smooth shock surface, this gives a first indication of the geometry of the shock, so that: <ul> <li>45∘<θBn<135∘: quasi-perpendicular shock condition</li> <li>θBn≤45∘ and θBn\(\geq\)135∘: quasi-parallel shock condition</li> </ul> Uncertainty on these angles is estimated to be ± 5º.  For details, see Simon Wedlund et al. (2022) above, §2.3 pp. 10-12. VARIABLES DESCRIPTION This database contains the following ASCII variables: <ul> <li>Bow shock times in Venus Express' database (1-s resolution): Tbs</li> <li>Venus Solar Orbital coordinates of the shock, in units of Venus radius RV (RV = 6051.8 km): XVSO, YVSO, ZVSO and Euclidean distance \(R_{VSO} = \sqrt{X_{VSO}^2 + Y_{VSO}^2 + Z_{VSO}^2}\) (in RV)</li> <li>Solar Zenith angle in degrees: SZA = \(\tan^{-1}{Y_{VSO}^2+Z_{VSO}^2 \over X_{VSO}^2}\) (in º) </li> <li>Angle between average B-field direction and shock normal assuming a smooth shock surface \(\theta_{Bn}\) (ThetaBn, in º, calculated with atan2(norm(cross(B,ñ),dot(B,ñ)), with B the magnetic field vector and ñ the vector normal to the shock surface): <ul> <li>45 < ThetaBn <  135 deg: quasi-\(\perp\) shock</li> <li>ThetaBn \(\leq\) 45 deg & ThetaBn \(\geq\) 135 deg: quasi-|| shock</li> </ul> </li> <li>Interplanetary Magnetic Field (IMF) upstream average vector in VSO coordinates, Bx, By, Bz (in nT).</li> <li>Flag for direction of crossing: <ul> <li>flag = 0: magnetosheath \(\longrightarrow\) solar wind (2447 events)</li> <li>flag = 1: solar wind \(\longrightarrow\) magnetosheath (2503 events)</li> </ul> </li> </ul> WARNING <ol> <li>This version of the database is currently in a preliminary stage of application and, as such, is not fully tested. Solar wind upstream magnetic field values (IMF) are given only as a first approximation for each orbit segment. See point 2 for caveats. For carefully manually picked shock crossings, the user is referred to the database of: Persson et al. (2023), Venusian bow shock crossings manually identified from measurements by the ASPERA-4 and MAG instruments onboard Venus Express, Zenodo (<a href="http://doi.org/10.5281/zenodo.7679677">https://doi.org/10.5281/zenodo.7679677</a>)</li> <li>This database is based on an automatic statistical geometrical estimate, further refined by constraints on magnetic fields. This is aimed at giving a first approximation of the shock area times in the Venus Express data. It is particularly suited to statistical studies and region identification in the Venus Express datasets. As such, this database should be used as a first indicator of the shock location, and with caution: it CANNOT, and WILL NOT substitute, especially in case studies, for a careful analysis of the full magnetometer and plasma bow shock signatures. Moreover, the algorithm is optimised for detecting the first disturbance observed in the magnetic field immediately ahead of the shock's foot (in the foreshock area), and not for the detection of other structures in the shock, such as the shock ramp. The "shock" location is therefore given here with typical uncertainties of about 0.040 RV (with RV = 6051.8 km, i.e., about 250 km in the radial direction). Finally, for multiple shock crossings, the algorithm chooses the first occurrence of the shock starting from the undisturbed solar wind.</li> </ol> Current formatting optimised for MATLAB. ACKNOWLEDGEMENTS C. Simon Wedlund and M. Volwerk thank the Austrian Science Fund (FWF) project P32035-N36.     LICENSE AND RIGHTS This database is shared under a Creative Commons CC-BY-4.0 license. Version 1 (c) Cyril Simon Wedlund @ Space Research Institute of Graz (IWF),                                                              Austrian Academy of Sciences, 2022-10-05 Contact email:        cyril.simon.wedlund@gmail.com

opencc-by-4.0Feb 2023View details →

zenodo44/100

Predicted times, spatial coordinates of bow shock crossings and shock geometry at Mars from the NASA/MAVEN mission, using spacecraft ephemerides and magnetic field data, with a predictor-corrector algorithm

CHARACTERISTICS Planet: Mars Radius: RM = 3389.5 km (volumetric mean planetary radius) Spacecraft: NASA/Mars Atmosphere and Volatile Evolution (MAVEN) Spacecraft coordinates system: Mars Solar Orbital (MSO) equivalent to Sun-State coordinate system: <ul> <li>+XMSO points towards the Sun from the planet’s centre,</li> <li>+ZMSO towards Mars’ North pole and perpendicular to the orbital plane defined as the XMSO–YMSO plane passing through the centre of Mars,</li> <li>YMSO completes the orthogonal system.</li> </ul> Time span: 01/11/2014 to 30/04/2024 (Mars Years MY32 to MY36 included, part of MY37). Total number N of candidate bow shock crossings in the database: N = 20107 ORIGINAL DATASETS USED The original MAVEN/MAG data repository on which these algorithms were applied is available on NASA's Planetary Data System (PDS) at <a href="https://doi.org/10.17189/1414178">https://doi.org/10.17189/1414178</a>. For this study, 1-Hz magnetic field data was used. METHOD To construct this database from the original datasets above, the predictor and predictor-corrector algorithms used are described in: Simon Wedlund, C., Volwerk, M., Beth, A., Mazelle, C., Möstl, C., Halekas, J., Gruesbeck, J. and Rojas-Castillo, D., (2022), A Fast Bow Shock Location Predictor-Estimator From 2D and 3D Analytical Models: Application to Mars and the MAVEN mission, Journal of Geophysical Research, 127, 1-33, e2021JA029942, <a href="https://doi. org/10.1029/2021JA029942">https://doi. org/10.1029/2021JA029942</a>.  Also available at: <a href="https://doi.org/10.1002/essoar.10507942.1">https://doi.org/10.1002/essoar.10507942.1 </a> and as arXiv e-print: <a href="https://doi.org/10.48550/arXiv.2109.04366">https://doi.org/10.48550/arXiv.2109.04366</a> These algorithms consist of two consecutive steps:  <ol> <li>Predictor geometric algorithm based on J. Gruesbeck's 3D model (<a href="https://doi.org/10.1029/2018JA025366">Gruesbeck et al. 2018</a>) for prediction of Mars bow shock position</li> <li>Corrector algorithm based on magnetic field measurements (magnitude and fluctuations).</li> </ol> REMARK ON VERSIONS From Version 3 onwards, we also provide the angle between the average Interplanetary Magnetic Field (IMF) vector upstream of the shock and the shock normal, noted \(\theta_{Bn}\)(ThetaBn). Assuming a smooth shock surface and the 3D model of Gruesbeck et al. (2018, all points), this gives a first indication of the geometry of the shock, so that: <ul> <li>45∘<θBn<135∘: quasi-perpendicular shock condition</li> <li>θBn≤45∘ and θBn≥135∘: quasi-parallel shock condition</li> </ul> Uncertainty on these angles is estimated to be ± 5º.  From Version 4 onwards, we also added the solar longitude Ls (in degrees). For details, see Simon Wedlund et al. (2022) above, §2.3 pp. 10-12. Note that due to minor adjustments in the code, some of the ThetaBn angles calculated here for the examples of Fig. 6 in Simon Wedlund et al. (2022) may slightly differ from the values quoted in the paper. VARIABLES DESCRIPTION This database contains the following ASCII variables: <ul> <li>Bow shock times in MAVEN's database (1-s resolution): Tbs</li> <li>Mars Solar Orbital coordinates of the shock, in units of Mars radius RM (RM = 3389.5 km): XMSO, YMSO, ZMSO and Euclidean distance \(R_{MSO} = \sqrt{X_{MSO}^2 + Y_{MSO}^2 + Z_{MSO}^2}\) (in RM)</li> <li>Solar Zenith angle in degrees: SZA = \(\tan^{-1}{Y_{MSO}^2+Z_{MSO}^2 \over X_{MSO}^2}\) (in º) </li> <li>Angle between average B-field direction and shock normal assuming a smooth shock surface \(\theta_{Bn}\) (ThetaBn, in º) <ul> <li>45 < ThetaBn <  135 deg: quasi-&perp; shock</li> <li>ThetaBn ≤45 deg & ThetaBn ≥ 135 deg: quasi-|| shock</li> </ul> </li> <li>Solar longitude Ls, in degrees.</li> <li>Flag for crossing: <ul> <li>sheath \(\longrightarrow\) solar wind, flag = 0.</li> <li>solar wind \(\longrightarrow\) sheath, flag = 1.</li> </ul> </li> </ul> WARNING This database is based on an automatic statistical geometrical estimate, further refined by constraints on magnetic field. It is aimed at giving a first approximation of the shock area times in the MAVEN data. It is particularly suited to statistical studies and region identification in the MAVEN datasets. As such, this database should be used as a first indicator of the shock location, and with caution: it CANNOT, and WILL NOT substitute, especially in case studies, for a careful analysis of the full magnetometer and plasma suite bow shock signatures. Moreover, the algorithm is optimised for detecting the first disturbance observed in the magnetic field immediately ahead of the shock's foot (in the foreshock area), and not for the detection of other structures in the shock, such as the shock ramp. The "shock" location is therefore given here with typical uncertainties of about 0.075 RM (with RM = 3389.5 km, i.e., about 250 km in the radial direction). Finally, for multiple shock crossings, the algorithm chooses the first occurrence of the shock starting from the undisturbed solar wind. Current formatting optimised for MATLAB. ACKNOWLEDGEMENTS C. Simon Wedlund and M. Volwerk thank the Austrian Science Fund (FWF) project P32035-N36. C. Möstl thanks the Austrian Science Fund FWF projects P31659-N27, P31521-N27. A. Beth thanks the Swedish National Space Agency (SNSA) and its support with the grant 108/18. This database was notably used to add to the Helio4Cast database which monitors solar wind parameters in the solar system (<a href="https://doi.org/10.6084/m9.figshare.6356420">https://doi.org/10.6084/m9.figshare.6356420</a>). Helio4Cast is available at <a href="http://www.helioforecast.space/icmecat">www.helioforecast.space/icmeca</a>t and <a href="http://www.helioforecast.space/sircat">www.helioforecast.space/sircat</a>.      LICENSE AND RIGHTS This database is shared under a Creative Commons CC-BY-4.0 license. Version 1 (c) Cyril Simon Wedlund @ Space Research Institute of Graz (IWF),                                                              Austrian Academy of Sciences (ÖAW), 2021-09-08 Version 2 (c) CSW @ ÖAW/IWF, 2021-11-30 -- Addition of R_MSO and SZA Version 3 (c) CSW @ ÖAW/IWF, 2022-02-09 -- Addition of ThetaBn Version 4 (c) CSW @ ÖAW/IWF, 2025-03-20 -- Addition of Ls, Bx, By, Bz and Bt.   Contact email:        cyril.simon.wedlund@gmail.com

opencc-by-4.0Nov 2021View details →

zenodo44/100

Lists of magnetopause and bow shock crossings, as measured by Juno/Waves and Juno/MAG.

Lists of magnetopause (boundary_crossings_caracteristics_MP.pdf, boundary_crossings_caracteristics_MP.csv) and bow shock crossings (boundary_crossings_caracteristics_BS.pdf, boundary_crossings_caracteristics_BS.csv), as measured by Juno/Waves and Juno/MAG (see below to download the files). For each crossing, number of the crossing (MP#), day of the year (DOY), date (year/month/day format) and time (hours:minutes format) are indicated, as well as the boundary crossed (magnetopause in this case), the direction of the crossing (in: from the magnetosphere to the magnetosheath; out: from the magnetosheath to the magnetosphere). The column “Notes” indicates whether the magnetopause has potentially not been completely crossed (see Fig. 1c of the article). Position of the crossings are given in the Cartesian JSS (Jupiter-‐De-Spun-Sun) and IAU (International Astronomical Union) coordinate systems, and IAU spherical coordinates system. Finally, the dynamic pressure of the solar wind, and the standoff distance of the magnetopause and the bow shock, derived from the model of Joy et al. (2002), are given in the last three columns. header = ['#',    "Day of Year",    "Date (year/month/day)",    "Time (HH:MM)",    "Boundary",    "In/Out",    "Notes",    "x (JSS)",    "y (JSS)",    "z (JSS)", "x (IAU)",    "y(IAU)",    "z (IAU)",    "r (IAU)",    "theta (IAU)",    "phi (IAU)",    "Dynamic Pressure (nPa)",    "Magnetopause Standoff Distance (Jovian radius)",    "Bow Shock Standoff Distance (Jovian radius)"] A python function to read the lists is provided (read_boundary_crossings_list.py). Example: <pre><code class="language-python">from read_boundary_crossings_list import * (header, indice, date, boundary, direction_crossing, notes, xyz_jss, xyz_iau, rtp_iau, pdyn, standoff_dist_mp, standoff_dist_bs) = read_boundary_crossings_list("boundary_crossings_caracteristics_MP.csv")</code></pre>   This dataset is linked to the following publication: Louis, C. K., Jackman, C. M., Hospodarsky, G., O’Kane Hackett, A., Devon-Hurley, E., Zarka, P., et al. (2023). Effect of a magnetospheric compression on Jovian radio emissions: In situ case study using Juno data. Journal of Geophysical Research: Space Physics, 128, e2022JA031155. <a href="https://doi.org/10.1029/2022JA031155">https://doi.org/10.1029/2022JA031155</a>

opencc-by-4.0Nov 2022View details →

zenodo44/100

Lists of Magnetopause and Bow Shock Crossings of Mercury by MESSENGER Spacecraft

The dataset titled “Lists of Magnetopause and Bow Shock Crossings of Mercury by MESSENGER Spacecraft” employs the measurements from the MESSENGER spacecraft’s Magnetometer (MAG) and Fast Imaging Plasma Spectrometer (FPIS) instruments to identify magnetopause and bow shock crossings during MESSENGER's orbit of Mercury. MESSENGER's data orbiting Mercury were collected between 23-03-2011 and 30-04-2015 and are available from the Planetary Data System’s Planetary Plasma Interactions (PDS/PPI) Node at https://pds-ppi.igpp.ucla.edu.   The dataset includes four lists: a, Bow_Shock_Out_Time_Duration_public_version_WeijieSun_20230829.txt b, Bow_Shock_In_Time_Duration__public_version_WeijieSun_20230829.txt c, MagPause_In_Time_Duration__public_version_WeijieSun_20230829.txt d, MagPause_Out_Time_Duration_public_version_WeijieSun_20230829.txt   Here are examples for the time in the list: Example A 2011 03 23 15 39 10.5  2011 03 23 16 24 02.4  BSO m  This entry represents multiple bow shock crossings. The first six columns indicate the time of the first boundary crossing, while the next six columns indicate the time of the last boundary crossing. “BSO” stands for outbound crossing of the bow shock, and “m” indicates that this is a multiple bow shock crossing made by MESSENGER. Only the first and last boundaries were selected out, we did not identify the boundary crossings in between.     Example B 2011 03 25 13 04 24.2  2011 03 25 13 04 24.0  BSI s  This entry represents a single bow shock crossing. The first six columns and the next six columns are identical, indicating that this is a single event. “BSI” stands for inbound crossing of the bow shock, and “s” indicates that this is a single bow shock crossing made by MESSENGER.   The dataset does not include magnetopause and bow shock crossings during the following time intervals: a. From 03:02 to 20:00 on 05-04-2011 b. From 24-05-2011 to 03-06-2011 c. From 17:50 to 22:53 on 16-04-2012 d. From 09-06-2012 to 13-06-2012 e. From 07:30 on 08-01-2013 to 16:00 on 09-01-2013 f. From 07:55 to 18:33 on 28-02-2013 g. From 14:22 to 17:38 on 26-12-2014   The current version is updated on 29 August 2023.   This work was supported by NASA Discovery Data Analysis Program (DDAP) Grant #80NSSC22K1061 (PI Weijie Sun).

opencc-by-4.0Aug 2023View details →

zenodo40/100

bow shock crossing data

The 595 bow shock crossings which were not included into the database used for developing the models of Lu et al. (2019) are used to compare the performance of the corresponding models. These test shock crossing data points are from Cluster 3 (2001–2008) and Cluster 4 (2001–2012). The corresponding interplanetary parameters for each bow shock crossing are taken from the OMNI data base (http://nssdc.gsfc.nasa.gov/omniweb/).

opencc-by-4.0Mar 2020View details →

zenodo40/100

Bow shock crossing list at Mercury (from MESSENGER magnetic field data)

<div> <div> <div> <div> Version 2 (latest):   This file contains a list of bow shock crossings at Mercury, identified from magnetic field data of the MESSENGER mission with 1 second resolution (not aberrated), (https://pds-ppi.igpp.ucla.edu/).  For a pre-selection of intervals containing bow shock crossings, we use the list of Philpott (2020): "MESSENGER bowshock and magnetopause crossings", https://doi.org/10.5683/SP2/1U6FEO. There, the first and last crossings of the inbound/outbound orbit segments are listed (boundary numbers 1 and 2 for inbound, 7 and 8 for outbound segments). For the bow shock identification, an automatic detection algorithm is applied to these intervals, extended by 45 seconds in either direction. The algorithm calculates running averages and variances of the magnetic field magnitude within adjacent 15 second intervals, separated by two seconds (gap interval). Whenever the ratio between the average magnetic fields exceed a threshold (default: 1.4), a bow shock crossing is selected. Should there be more than one ratio maximum within 10 seconds, then only the maximum is selected that corresponds to the minimal sum of the variances within the adjacent intervals. Crossings are classified with respect to detection quality depending on the ratios of the average magnetic fields and the corresponding variances. Details can be found in the algorithm script that is published alongside this file. Columns of the list file:  ['time', 'orbit_number', 'x_mso_km', 'y_mso_km', 'z_mso_km', 'jump_ratio', 'indicator'] 'time': date and time in YYYY-MM-DD HH:mm:SS 'orbit_number': orbit number (MESSENGER Mission) 'x_mso_km': position (x-coordinate) in MSO coordinate system in km, not aberrated 'y_mso_km': position (y-coordinate) in MSO coordinate system in km, not aberrated 'z_mso_km': position (z-coordinate) in MSO coordinate system in km, not aberrated 'in/out': inbound or outbound segment of the orbit (apoherm towards periherm or periherm towards apoherm) 'jump_ratio': ratio of the average magnetic fields before and after selected crossings 'indicator': 1, 2 or 3 (1: very clear crossings, high quality, 2: clear crossings, good quality, 3: unclear crossings, poor quality) For further analysis it is recommended to only use the crossings with the indicators 1 and 2. The uncertainty in the determination of the times is +/- 2 seconds.  Number of analyzed orbits: 3982 Number of total crossings found: 13502 Number of crossings with indicator 1 (very clear crossings, best quality): 1765 Number of crossings with indicator 2 (clear crossings, good quality): 5027 Number of crossings with indicator 3 (unclear crossings, poor quality): 6710   Version 1:  This file contains a list of bow shock crossings at Mercury, identified from magnetic field data of the MESSENGER mission with 1 second resolution (not aberrated), (https://pds-ppi.igpp.ucla.edu/).  For a pre-selection of intervals containing bow shock crossings, we use the list of Philpott (2020): "MESSENGER bowshock and magnetopause crossings", https://doi.org/10.5683/SP2/1U6FEO. There, the first and last crossings of the inbound/outbound orbit segments are listed (boundary numbers 1 and 2 for inbound, 7 and 8 for outbound segments). For the bow shock identification, an automatic detection algorithm is applied to these intervals, extended by 15 seconds in either direction. The algorithm calculates running averages and variances of the magnetic field magnitude within adjacent 15 second intervals, separated by two seconds (gap interval). Whenever the ratio between the average magnetic fields exceed a threshold (default: 1.4), a bow shock crossing is selected. Should there be more than one ratio maximum within 10 seconds, then only the maximum is selected that corresponds to the minimal sum of the variances within the adjacent intervals. Crossings are classified with respect to detection quality depending on the ratios of the average magnetic fields and the corresponding variances. Details can be found in the algorithm script that is published alongside this file. Columns of the list file:  ['time', 'orbit_number', 'x_mso_km', 'y_mso_km', 'z_mso_km', 'in/out', 'jump_ratio', 'indicator'] 'time': date and time in YYYY-MM-DD HH:mm:SS 'orbit_number': orbit number (MESSENGER Mission) 'x_mso_km': position (x-coordinate) in MSO coordinate system in km, not aberrated 'y_mso_km': position (y-coordinate) in MSO coordinate system in km, not aberrated 'z_mso_km': position (z-coordinate) in MSO coordinate system in km, not aberrated 'in/out': inbound or outbound segment of the orbit (apoherm towards periherm or periherm towards apoherm) 'jump_ratio': ratio of the average magnetic fields before and after selected crossings 'indicator': 1, 2 or 3 (1: very clear crossings, high quality, 2: clear crossings, good quality, 3: unclear crossings, poor quality) For further analysis it is recommended to only use the crossings with the indicators 1 and 2. The uncertainty in the determination of the times is +/- 2 seconds.  Number of analyzed orbits: 3982 Number of total crossings found: 65666 Number of crossings with indicator 1 (very clear crossings, best quality): 4291 Number of crossings with indicator 2 (clear crossings, good quality): 16652 Number of crossings with indicator 3 (unclear crossings, poor quality): 44723 </div> <div> </div> <div> </div> </div> </div> </div>

opencc-by-4.0Nov 2024View details →

zenodo40/100

List of Saturn magnetopause and bow shock crossings by the Cassini spacecraft

This is an updated list of magnetopause (MP) and bow shock (BS) crossings from Cassini, based on the list presented in Jackman et al. [2019] <a href="https://doi.org/10.1029/2019JA026628">https://doi.org/10.1029/2019JA026628</a>. This uploaded list has the following changes from the list first presented in that paper (and included in that supplementary material):   I = inbound O = outbound Amendments to Cassini MP/BS crossing list Changes made 26/01/2021 Total #MP crossings: 2118 (some times changed) Total #BS crossings: 1247 (3 pairs added, 1 pair removed, some times changed) Change list below: Change #1: Note the following crossings come from a list on MAPSView which was originally collated based on MAG and CAPS data.  MAG data gap spans these dates so crossings are based on other instruments at these times. ELS and SNG data available 2004 181-185 and 195-196 (except 196 13-23 UT). 2004    181    02    43    MP    I     2004    186    04    42    MP    O    2004    186    10    24    MP    I     2004    186    17    57    MP    O    2004    186    20    17    MP    I     2004    188    07    06    MP    O   2004    188    08    11    MP    I     2004    188    13    14    MP    O   2004    188    15    13    MP    I     2004    188    19    39    MP    O   2004    189    14    05    BS    O   2004    189    16    15    BS    I     2004    189    21    46    BS    O   2004    190    00    30    BS    I     2004    190    04    13    BS    O   2004    190    10    56    BS    I     2004    190    11    54    BS    O   2004    190    11    54    DG    S_SW  2004    194    05    12    DG    E_SH   2004    194    05    12    BS    O     2004    196    03    11    BS    I     2004    196    06    59    BS    O   Change #2: Change 2004    348    05    27    MP    I     to 2004    348    05    00    MP    I     Change #3: Added some crossings on 2004 day 345 2004 345 11 52 BS I 2004 345 11 58 BS O 2004 345 12 20 BS I 2004 345 12 26 BS O 2004 345 23 06 BS I 2004 345 23 13 BS O Change #4:  Changed 2004 day 345 13 24 BS I  to 2004 day 345 12 57 BS I Change #5:  Remove 2014    322    6    8    BS    I     2014    326    1    23    BS    O     _________________________________________________________________________________________ Additional changes made through discussion with Matthew Cheng, August 13th 2021 Original list: Master_BS_MP_Crossing_List_04_16_incCMJcorr_published 1st Revised list: Master_BS_MP_Crossing_List_04_16_incCMJcorr_revised 2nd Revised list: Master_BS_MP_Crossing_List_04_16_incCMJcorr_revised_120821 Since 1st revised list: Total #MP crossings: 2122 (2 new pairs, some times changed) Total #BS crossings: 1249 (1 new pair, some times changed) Change #6 Changed typo 2016    068    12    19    DG    E_MP         to 2016    068    12    19    DG    E_SP         Change #7 Change  2016    242    12    00    MP    O         To: 2016    242    11    15    MP    O     Change #8 Change  2016    152    16    33    BS    O to  2016    152    15    22    BS    O Change #9 Change  2016    153    02    24    BS    O     to     2016    153    02    08    BS    O         Change #10 Change  2016    153    12    00    BS    I         to 2016    153    11    45    BS    I         Change #11 Add new MP pair 2016    155    11    05    MP    O     2016    155    12    52    MP    I     Change #12 Change 2011    2    03    14    MP    O     to 2011    2    01    48    MP    O     Change #13 Change: 2012    145    15    11    MP    O     To 2012    145    14    36    MP    O Change #14 Changed 2007    33    16    25    MP    I     to  2007    33    15    25    MP    I     Change #15 Add new MP pair 2005    45    11    55    MP    O     2005    45    12    36    MP    I    Change #16 Add new BS pair 2012    277    00    15    BS    I     2012    277    01    36    BS    O Change #17 Add new MP pair 2008    85    14    31    MP    I   2008    85    15    38    MP    O

opencc-by-4.0Jan 2022View details →

zenodo40/100

A database of MMS bow shock crossings compiled using machine learning

We use a machine learning approach to automatically identify shock crossings from the Magnetospheric Multiscale (MMS) spacecraft. We compile a database of 2797 crossings including various spacecraft related and shock related parameters for each event. Furthermore, for each event we provide an overview plot containing key parameters of the shock crossing. A Technical report detailing the content of the database can be found at the DOI: http://dx.doi.org/10.1029/2022JA030454

opencc-by-4.0Mar 2022View details →

zenodo40/100

Venusian bow shock crossings manually identified from measurements by the ASPERA-4 and MAG instruments onboard Venus Express

Bow shock crossings at Venus identified manually from the ASPERA-4 and MAG instruments onboard Venus Express for the full mission from 2006 to 2014. A detailed description of the dataset can be found in the paper "Influence of solar wind variations on the shapes of Venus’ plasma boundaries based on Venus Express observations" by Signoles et al. The boundary crossings by Venus Express are determined from combining the measurements of both ion, electron and magnetic field measurements. The bow shock is identified from the sharp increase in the magnetic field magnitude, and the increase in electron and ion temperature. The ion composition boundary is identified from the decrease in magnetosheath protons and electrons, and the appearance of planetary heavy ions. The dataset contains 5193 identified bow shock crossings and 2679 identified ion composition boundary crossings. For more information on the dataset contact: M. Persson, moaperssonphd at gmail.com

opencc-by-4.0Mar 2023View details →

zenodo36/100

The identified bow shock crossings based on Venus Express observations

<div>Bow shock locations and upstream parameters observed by Venus Express.</div> <div> </div> <div>The columns are structured as follows:</div> <div>    1: time of bow shock crossings dd-mmm-yyyy HH:MM:SS</div> <div>    2: X-VSE [Rv]</div> <div>    3: Y-VSE [Rv]</div> <div>    4: Z-VSE [Rv]</div> <div>5: Solar wind magnetosonic Mach number</div> <div>    6: EUV [mW/m^2]</div> <div>    7: IMF Bx in VSE [nT]</div> <div>8: IMF By in VSE [nT]</div> <div>    9: IMF intensity |B| [nT]</div> <div>    10: IMF cone angle [degree]</div> <div>11: Solar wind dynamic pressure [nPa]</div> <div>12: The angle between the IMF and the shock normal, thetaBn [degree]</div> <div> </div> <div>Please contact xuqi01@nssc.ac.cn if you have questions.</div>

opencc-by-4.0Aug 2024View details →

zenodo36/100

List of Mercury's Bow Shock and Magnetopause Crossings by the MESSENGER Spacecraft

This dataset contains a list of Mercury’s bow shock and magnetopause boundary crossings by the MESSENGER spacecraft during its entire orbital mission, from March 23, 2011, to April 30, 2015. A total of 4,054 orbits were identified. The boundary crossings were visually identified by abrupt changes in the magnetic field strength and direction as the spacecraft traversed the current layer, assisted by a sharp boundary in the ion flux spectrogram between different regions. Due to the inward and outward motions of these boundaries, multiple crossings were typically observed. The dataset provides the innermost and outermost crossings for each pass.  File descriptions: *MP_in.dat*: Inbound magnetopause crossings. *MP_out.dat*: Outbound magnetopause crossings. *BS_in.dat*: Inbound bow shock crossings. *BS_out.dat*: Outbound bow shock crossings. Each file includes two columns: the time strings for the first and last crossings during each pass. For passes with only one crossing, the second time string is labeled as “NAN.” In a few orbits where the bow shock was not detected, both columns are labeled as “NAN.” The MESSENGER MAG and FIPS data used for the identification is publicly available via NASA’s Planetary Data System (https://pds-ppi.igpp.ucla.edu/). This dataset is linked to the following publications: Zhong et al. (2015), Mercury’s three-dimensional asymmetric magnetopause, J. Geophy. Res. Space Physics, 120, 7658–7671, <a href="https://doi.org/10.1002/2015JA021425">https://doi.org/10.1002/2015JA021425</a>. Zhong et al. (2015), Compressibility of Mercury’s dayside magnetosphere, Geophy. Res. Lett., 42(23), 10135-10139. <a href="https://doi.org/10.1002/2015GL067063">https://doi.org/10.1002/2015GL067063</a>. Zhong et al. (2020), Effects of Orbital Eccentricity and IMF Cone Angle on the Dimensions of Mercury’s Magnetosphere, Astrophys. J., 892(1), 2. 10135-10139. <a href="https://doi.org/10.3847/1538-4357/ab7819">https://doi.org/10.3847/1538-4357/ab7819</a>. Zhong & Wang, Global magnetic field properties in Mercury’s solar wind interaction from MESSENGER measurements [submitted, A&A, 2024].

opencc-by-4.0Oct 2024View details →

zenodo32/100

Supporting Information for "Terrestrial bow shock parameters from MMS measurements: dependence on upstream and downstream time ranges"

Summary plots and parameter tables for each of the 51 shocks analyzed in the statistical study "Terrestrial bow shock parameters from MMS measurements: dependence on upstream and downstream time ranges."

opencc-by-4.0Dec 2019View details →

zenodo32/100

Dataset for for manuscript "Solar wind magnetic holes can cross the bow shock and enter the magnetosheath"

This data set contains event times and basic properties of magnetic holes analysed in the manuscript "Solar wind magnetic holes can cross the bow shock and enter the magnetosheath".

opencc-by-4.0Jul 2022View details →

zenodo32/100

Bow shock ripples and their modulation of whistler wave packets: MMS observations

Dataset for the paper "Bow shock ripples and their modulation of whistler wave packets: MMS observations". The data are for the Figures 1 and 2 in the manuscript. These files can be processed by Matlab with the help of the IRFU-matlab package, which is available at https://github.com/irfu/irfu-matlab.

opencc-by-4.0Aug 2024View details →

nasa20/100

OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 5 min Data

Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 5 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005

restrictednotspecifiedApr 2025View details →

nasa20/100

OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 1 min Data

Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 1 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005

restrictednotspecifiedApr 2025View details →

nasa20/100

PVO VENUS ELECT TEMP PROBE DERVD BOW SHOCK LOCATION VER 1.0

The Bow Shock File. This file gives the orbit-by-orbit times and locations of the bow shock crossings, which are characterized by distinct changes in Ne. Multiple shock crossing are listed if they are sufficiently separated to be resolved accurately. (Bow shock crossings will be evident in the High Resolution Ne File when they occurred within 30 minutes of periapsis)

restrictedus-pdMar 2025View details →

nasa12/100

PVO VENUS ELECT TEMP PROBE DERVD BOW SHOCK LOCATION VER 1.0

restrictednotspecifiedMar 2025View details →

nasa12/100

Wind Magnetic Field Investigation (MFI) Solar Wind Experiment (SWE) 1-min field and plasma data at bow shock nose

Solar wind magnetic field and plasma data at 1-min resolution created from Wind data shifted to the Earth's bow shock nose (BSN).

restrictednotspecifiedAug 2025View details →

nasa8/100

ISEE 1 FPE plasma parameters, 6 Re to bow shock

TBD

restrictednotspecifiedApr 2025View details →

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Last verified 2026-04-30Open record

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Last verified 2026-04-29Open record

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Last verified 2026-04-29Open record