{"id":"08ba701a-df09-4ed9-8326-a32ff5818f66","arxiv_id":"2506.19986","paper_version":1,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":4.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":5,"one_line_summary":"Using Solar Orbiter SWA-PAS and MAG data, the authors identify 44 interplanetary shocks in 2023, mostly fast forward, and report that their rate increased with heliocentric distance.","lead":"This paper applies a threshold-based algorithm to Solar Orbiter plasma and magnetic field data from 2023 and reports 44 interplanetary shock waves with estimated speeds, compression ratios, and angles. A smart generalist might read it as a test of whether automated shock catalogs can be extended to a new solar cycle and spacecraft orbit.","discovery_kind":"extension","skeptic_critique":{"model":"deepseek-v4-flash","headline":"Table 2 lists shock candidates with Mfms<1 (events #5, #11, #22), which is physically impossible for a shock; Eq. (15) omits V_sh, so the Mach numbers are not shock-frame values and the catalog's internal consistency is broken.","rationale":"The reader's weakest_assumption concerns in-sample threshold selection and the absence of event-by-event validation against ipshocks and Serpentine. That concern is legitimate, but the most load-bearing problem is internal: the paper's own Table 2 contains events with fast-magnetosonic Mach numbers below 1, which contradicts the definition of a shock. The reader mentioned this issue in the rationale, but did not make it the primary weakest assumption. I therefore agree partially: external validation is necessary, but the internal Mach-number inconsistency is more direct and can be checked immediately from the provided tables. The likely cause is Eq. (15), which omits the shock velocity V_sh, so the reported Mfms values are not evaluated in the shock frame. This affects the central claim of 44 IP shocks and all derived statistical trends, including Fig. 7. The proposed concrete test distinguishes the two failure modes: a wrong formula versus false-positive detections. Since the issue is fixable and the rest of the catalog may still be largely valid, the reader's CONDITIONAL verdict remains appropriate; no change in verdict is needed.","tokens_in":16715,"tokens_out":5057,"duration_ms":50100,"concrete_test":"Recompute Mfms and MA for events #5, #11, and #22 with M_fms = |V_sh − V_us·n| / V_fms, using the upstream normal velocity V_us·n from the 4-s SWA-PAS L2 data and the V_sh, V_fms values in Table 2; then check whether the same events appear in the ipshocks or Serpentine SolO list. If any event remains Mfms < 1 and is absent from both databases, it is a false positive and should be removed before recomputing Fig. 7; if it appears in the databases with Mfms > 1, Eq. (15) is the error and must be corrected.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The paper's central claim is that the algorithm identified 44 true IP shocks in 2023. The strongest internal check on that claim is the Mach-number table: a fast-mode shock requires Mfms > 1 in the upstream medium, yet Table 2 reports Mfms = 0.72 (event #5), 0.41 (#11), and 0.76 (#22), with MA < 1 for #5 and #11 as well. These entries are sub-magnetosonic and cannot satisfy the paper's own definition of a shock. The likely source is Eq. (15), which defines Mfms = |V_us·n| / V_fms and omits the shock speed V_sh computed in Eq. (11); the fast-magnetosonic Mach number must be evaluated in the shock frame, |V_sh - V_us·n| / V_fms. If the formula is wrong, all Mach numbers and the statistics built on them are unreliable. If the formula is right, those events are not shocks and the catalog membership is wrong. Either way, the load-bearing claim '44 IP shocks' is not internally consistent, independently of any comparison with external databases.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper presents a semi-automated shock detection algorithm adapted from Kruparova et al. (2013) and applies it to Solar Orbiter SWA-PAS and MAG data for the full year 2023, identifying 44 interplanetary shocks (40 fast-forward, 2 fast-reverse, 1 slow-forward, 1 slow-reverse) at heliocentric distances of 0.29–0.95 AU. For each event, the paper reports compression ratios, quality factors, upstream plasma beta, shock-normal angle, Alfvén speed, sound speed, fast-magnetosonic speed, and Mach numbers. It also presents distributions of theta_Bn and beta_us, and a heliocentric-distance-normalized shock rate that is claimed to increase with radial distance.","tokens_in":16991,"tokens_out":6241,"duration_ms":63950,"significance":"If the catalog and its parameters are reliable, the paper would provide a useful addition to interplanetary-shock statistics in the ascending phase of solar cycle 25, exploiting Solar Orbiter's unique inner-heliospheric coverage. Strengths include the use of high-resolution SWA-PAS and MAG data, the public presentation of a 44-event list with parameters, and the comparison of aggregate event counts with the ipshocks and Serpentine databases. However, the central claim is not currently supported because the detection thresholds are chosen in-sample from the same candidates that form the final list, and Table 2 contains events with fast-magnetosonic Mach numbers below 1, which is physically impossible for a shock. These issues bear directly on catalog membership, all derived parameter statistics, and the reported radial trend, so they must be resolved before the results can be accepted.","major_comments":[{"comment":"The detection thresholds (delta_N > 0.35, delta_V > 0.05, delta_B > 0.30, QF1 > 0.25, QF2 > 0.15) are obtained by inspecting histograms of the same ~50 candidates that are subsequently filtered into the final 44-event list. This is an in-sample threshold choice with no independent validation set. The comparison with ipshocks and Serpentine totals (35 and 43 events) is aggregate only, not event-by-event, so it does not establish that the 44 events are true shocks or that the type mix is correct. The catalog membership and all derived distributions are therefore partly a restatement of the threshold choices. Please provide an out-of-sample validation (e.g., event-by-event comparison with the Serpentine or ipshocks lists) or a sensitivity analysis showing the catalog is stable under reasonable threshold variations.","section":"Section 3.1, Figures 1–2"},{"comment":"Equation (15) defines Mfms = |V_us·n| / V_fms, omitting the shock speed V_sh computed in Eq. (11). The fast-magnetosonic Mach number must be evaluated in the shock frame, i.e., |V_sh − V_us·n| / V_fms (with an appropriate sign convention). As written, Eq. (15) yields Mfms < 1 for events #5 (0.72), #11 (0.41), and #22 (0.76), which is physically impossible for a fast shock and contradicts the paper's own identification of these events as FF/SR shocks. Either the formula is wrong, in which case all Mach numbers in Table 2 and all statistics based on them are unreliable, or these events are not shocks, in which case the catalog contains false positives. Please correct Eq. (15) (and the ambiguous ± sign in Eq. (14)) and recompute the Mach numbers, then re-examine whether the remaining events satisfy Mfms > 1 and MA > 1.","section":"Section 3.2, Eq. (15) and Table 2"},{"comment":"No uncertainties are given for theta_Bn, V_sh, MA, or Mfms. The MX3 single-spacecraft normal method is sensitive to the choice of upstream/downstream averaging windows and to noise, and the paper itself notes that the 5-minute window was chosen after trying 5–10 minute intervals. Because the paper's statistical conclusions (e.g., the peak at theta_Bn ~ 50° in Fig. 5a and the claim that most shocks are quasi-perpendicular) depend on these point estimates, please provide error bars or a sensitivity analysis over averaging windows and normal-method variants.","section":"Section 3.2, Tables 1–2"},{"comment":"The claim that the distance-normalized shock rate N_IP_Rd increases with Rd is based on 44 events divided into 10 bins, and the authors note that one strong event at ~0.63 AU dominates the parameter maxima. The paper does not test whether the radial trend is robust to the threshold choices or to removal of outlier events, nor does it account for the small number of events per bin after normalization. Please provide Poisson error bars and a robustness check of the trend, for example by recomputing the rate with alternative thresholds or by excluding the dominant event.","section":"Section 3.4, Figure 7"}],"minor_comments":[{"comment":"The expression for V_fms is dimensionally incorrect as written (the factor 1/2 is placed outside instead of taking the square root of the whole expression). The numerical values in Table 2 suggest the intended formula was used, so please fix this typographical error.","section":"Eq. (16)"},{"comment":"The ± sign before V_sh in Eq. (14) is ambiguous; please specify the sign convention for forward and reverse shocks and how it relates to V_sh from Eq. (11).","section":"Eq. (14)"},{"comment":"The histogram in Fig. 5a is described as showing the largest counts at theta_Bn ~ 50°, but the bin width and the sample size per bin are not stated; please provide these details for clarity.","section":"Section 3.3, Fig. 5a"},{"comment":"The abstract says 'over 40 IP-shock waves' while the text specifies 44; please use consistent numbers throughout.","section":"Abstract and Section 3.2"},{"comment":"The column 'Angle S–E' is only defined in Annex C, not in the main text; this makes Table 1 difficult to interpret without jumping to the annex.","section":"Table 1 and Annex C"},{"comment":"The comparison with the ipshocks and Serpentine databases should state the version or access date of the catalogs used, because these lists are updated over time.","section":"Section 3.2 and References"}],"recommendation":"major_revision","confidential_remarks":"The manuscript appears to be a near-final provisional PDF, but the scientific content is not yet fully sound. The Mach-number inconsistency in Eq. (15) and Table 2 is a load-bearing error that must be corrected, and the in-sample threshold selection needs an out-of-sample validation or sensitivity analysis. If the authors can fix these points, the paper could be publishable as a catalog/statistical study, but in its current form the central claims are not sufficiently supported."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Elena — quick take on Yakovlev et al. 2506.19986. The new piece is a 2023 Solar Orbiter shock list: 44 events with compression ratios, shock types, theta_Bn, beta, and Mach numbers. The detection logic is Kruparova's 2013 algorithm with retuned thresholds, and the list overlaps with ipshocks and Serpentine, so the novelty is modest. Still, a year-specific catalog with parameter tables is a legitimate data contribution, and the aggregate comparison with existing databases is a good instinct.\n\nThe paper does some things well. The methodology is transparent: they state the thresholds, show the candidate histograms, and list every event in Annexes. Using fixed 5-minute upstream/downstream windows is a reasonable choice, and they acknowledge the averaging-window literature. They also normalize the shock rate by the time spent at each heliocentric distance, which is more careful than some catalog papers.\n\nThe soft spots are real. First, the thresholds in Section 3.1 are selected from histograms of the same ~50 candidates that produce the final 44-event list, so the catalog is partly a restatement of those choices. There is no event-by-event validation against ipshocks or Serpentine, only a total-count comparison. Second, and more serious, the Mach-number table is internally broken. Events #5, #11, and #22 have Mfms < 1 (0.72, 0.41, 0.76), which cannot be fast-mode shocks by the paper's own standard. The likely source is Eq. (15), which defines Mfms = |V_us·n| / V_fms and drops the shock speed V_sh that appears in Eq. (14) for MA. The fast magnetosonic Mach number must be evaluated in the shock frame: |V_sh - V_us·n| / V_fms. If the formula is wrong, all Mfms values and any statistics built on them are unreliable. If it's right, those three events are not shocks. Either way, the '44 IP shocks' claim needs attention.\n\nMinor issues: no uncertainties on shock normals or Mach numbers (single-spacecraft methods have significant error bars), and the outward increase in normalized shock rate could still be partly a selection effect near perihelion; the authors mention spatial coverage but don't quantify it.\n\nWho is this for? Space-weather modelers and shock-catalog builders who want a 2023 SolO list and don't mind tracing events themselves. It deserves a serious referee, but only with major revision: fix the Mach formula, re-examine the sub-magnetosonic events, and add an event-by-event comparison to existing catalogs. If the list holds up after that, it's a usable contribution. As it stands, I'd be careful citing the parameter tables.","headline":"A potentially useful 2023 SolO shock catalog is undercut by a Mach-number formula that omits the shock speed, producing three sub-magnetosonic 'shocks' in the table.","tokens_in":17530,"tokens_out":3874,"would_cite":false,"duration_ms":46086,"reading_group":"maybe","serious_thinker":"no","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"This paper claims that a semi-automated algorithm built on simultaneous jumps in density, speed, and magnetic field detects 44 interplanetary shocks in Solar Orbiter data during 2023, and that the rate of shocks per observing time rises…","keywords":["interplanetary shocks","solar wind","Solar Orbiter","shock detection algorithm","shock Mach number","plasma beta","heliocentric distance","solar cycle 25"],"falsifier":"Compare the 44 claimed events one by one against the raw Solar Orbiter L2 data and against independent shock identifications for the same spacecraft and dates; if many claimed shocks lack simultaneous jumps in density, speed, and magnetic field above the stated thresholds, or if events listed in independent catalogs are systematically missing, the central claim is undermined.","tokens_in":16520,"feed_emoji":"☀️","tokens_out":5284,"duration_ms":48520,"temperature":0.7,"pith_summary":"This paper adapts a previously published automated shock-detection algorithm to data from Solar Orbiter's proton sensor and magnetometer and applies it to the whole year 2023, when the spacecraft was between 0.29 and 0.95 AU from the Sun. The authors report 44 interplanetary shocks—40 fast forward, 2 fast reverse, 1 slow forward, and 1 slow reverse—and tabulate their compression ratios, Mach numbers, upstream plasma beta, and the angle between the shock normal and magnetic field. Most shocks are quasiperpendicular, with the angle peaked near 50 degrees, and most have upstream beta below 1, indicating magnetic-field-dominated dynamics. After normalizing by the time the spacecraft spent in each radial distance segment, the number of shocks per unit time increases toward larger heliocentric distances. The result is a year-long, instrument-specific shock catalog from the ascending phase of solar cycle 25, providing a basis for space-weather and shock-acceleration studies.","feed_headline":"Solar Orbiter data yield 44 interplanetary shocks for 2023","feed_subtitle":"Most are fast forward and quasiperpendicular; normalized shock rate climbs with distance from the Sun.","key_machinery":"The detection machinery is a set of relative step-change thresholds applied to a 300-second sliding window: density change ΔN > 0.35, speed change ΔV > 0.05, and magnetic-field magnitude change ΔB > 0.30, combined with two quality factors QF1 = (ΔB + ΔN + ΔV)/3 and QF2 = ΔB/4 + ΔN/12 + 2ΔV/3 exceeding 0.25 and 0.15, plus auxiliary conditions that the changes occur simultaneously and that the downstream speed is lower than the upstream speed. Shock parameters are then derived from 5-minute upstream and downstream averages using standard single-spacecraft techniques, including magnetic-field and density compression ratios, upstream plasma beta, Alfvén Mach number, and the shock-normal angle via a magnetic coplanarity method.","core_discovery":"Using simultaneous step changes in proton density, speed, and magnetic-field magnitude, combined with two quality factors, the authors claim to have detected 44 interplanetary shocks in Solar Orbiter data during 2023. The catalog's composition is strongly dominated by fast forward shocks (40 of 44). The statistical distributions show that the angle between the shock normal and the upstream magnetic field clusters around 50 degrees, so most events are quasiperpendicular, and upstream plasma beta is below unity for the majority of events. After dividing the heliocentric distance range into ten equal segments and normalizing the shock count by the time spent in each segment, the normalized shock frequency increases with distance from the Sun. The authors also report that compression ratios and quality factors peak around 0.63 AU, tied to one strong event rather than a statistically averaged trend.","pith_inferences":["Event-by-event agreement with the independent catalogs the paper cites would test whether the algorithm's extra sensitivity is real or an artifact of threshold choices; the paper only compares aggregate counts, not individual events.","Because the thresholds were chosen from the same candidate set that produced the final list, the reported increase of shock rate with distance could partly reflect selection effects; applying the algorithm to 2024 data would show whether the thresholds transfer to an independent period.","The few events with extreme parameters, such as the one with Alfvén Mach number near 25, may be attractive targets for dedicated studies of particle acceleration, similar to other high-Mach-number shocks discussed in the literature.","Connecting each shock time to the flare and coronal mass ejection lists the paper begins to use could test whether the local peak in shock parameters around 0.63 AU is associated with a specific solar eruption, a hypothesis the authors raise but do not fully verify."],"forward_implications":["The 44-event list provides a reference set of interplanetary shocks in the ascending phase of solar cycle 25 at heliocentric distances of 0.29 to 0.95 AU.","The strong dominance of fast forward shocks and quasiperpendicular geometries can be compared with shock populations observed at other phases of the solar cycle and by other missions.","The increasing normalized shock rate with distance supports the picture that the observed shock count grows as the spacecraft's whole-sky spatial coverage in the Sunward direction expands and as CME-driven shocks develop further from the Sun.","The stated thresholds and algorithm can be applied to Solar Orbiter data from later years to track how shock properties evolve through solar cycle 25.","The finding that most events have upstream plasma beta below 1 indicates that magnetic pressure dominates thermal pressure at these shock fronts, which matters for particle-acceleration models.","The comparison with publicly documented shock counts for the same year gives a quick consistency check, though the aggregate numbers differ by up to nine events."],"supporting_citations":[{"why":"Supplies the base automated shock-detection algorithm and quality-factor definitions that the paper adapts with new thresholds.","marker":"Kruparova 2013"},{"why":"Describes the SWA-PAS instrument whose proton density, speed, and temperature data are used for the analysis.","marker":"Owen 2020"},{"why":"Describes the MAG instrument whose magnetic-field measurements provide the IMF magnitude and components.","marker":"Horbury 2020"},{"why":"Provides the standard formulas the paper uses for shock normals, Mach numbers, and related parameters.","marker":"Schwartz 1998"},{"why":"Provides the Helsinki shock database conventions and typical shock parameter estimation methods that the paper follows and compares against.","marker":"Kilpua et al. 2015"},{"why":"Analyzes how upstream and downstream averaging windows affect shock parameter estimates, guiding the choice of 5-minute windows.","marker":"Trotta et al. 2022"},{"why":"Provides an earlier automated shock search in Solar Orbiter data (2020–2022) whose event count is compared with the 2023 result.","marker":"Dimmock et al. 2023"},{"why":"Provides the Zenodo version of the Solar Orbiter cycle 25 shock list that the paper compares with its own 2023 events.","marker":"Trotta et al. 2024b"}],"fun_headline_variants":["Solar Orbiter sees 44 interplanetary shocks in 2023","Shock frequency climbs with distance in Solar Orbiter data","44 shocks cataloged by Solar Orbiter, mostly fast forward","Quasiperpendicular shocks dominate Solar Orbiter 2023 catalog","Solar Orbiter 2023 shock survey: 44 events, rate rises"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The detection thresholds were picked by inspecting histograms of the same set of roughly 50 candidate events that later produced the 44-shock list, so the catalog membership and the reported distance trend rest on thresholds that were not checked against an independent, labeled sample.","fun_headline_variants_meta":{"raw":{"variants":["Solar Orbiter sees 44 interplanetary shocks in 2023","Shock frequency climbs with distance in Solar Orbiter data","44 shocks cataloged by Solar Orbiter, mostly fast forward","Quasiperpendicular shocks dominate Solar Orbiter 2023 catalog","Solar Orbiter 2023 shock survey: 44 events, rate rises"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000311,"raw_usage":{"total_tokens":1829,"prompt_tokens":1059,"completion_tokens":770,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":675,"completion_tokens_details":{"reasoning_tokens":679}},"tokens_in":675,"tokens_out":770,"duration_ms":7370,"temperature":1.0,"reasoning_tokens":679,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-06T22:59:23.270419+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Compare the 44 claimed events one by one against the raw Solar Orbiter L2 data and against independent shock identifications for the same spacecraft and dates; if many claimed shocks lack simultaneous jumps in density, speed, and magnetic field above the stated thresholds, or if events listed in independent catalogs are systematically missing, the central claim is undermined.","supporting_citations":[],"review_version":1}