{"id":"7173f848-d919-4e9e-a55d-109d497b5645","arxiv_id":"2501.05337","paper_version":1,"verdict":"CONDITIONAL","confidence":"HIGH","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":3,"one_line_summary":"Over one Martian year, Jezero pressure shows thermal tides up to six harmonics and 2-4 sol waves whose amplitude grows with dust; four dust storms caused tide amplitude increases with inverse phase responses.","lead":"Perseverance surface pressure data and orbital images are combined to characterize atmospheric disturbances at Jezero Crater across a full Martian year. The study links thermal tides, dust storms, and 2-4 sol baroclinic wave activity, showing how dust modifies pressure oscillations.","discovery_kind":"extension","skeptic_critique":{"model":"deepseek-v4-flash","headline":"Model 'agreement' for baroclinic waves is not a free prediction: the PCM run in §7.2 is nudged with observed MY36 dust maps, so it cannot independently validate the wave–dust trend.","rationale":"Reader's weakest assumption correctly identifies the prescribed-dust forcing. My independent reading of §7.2 confirms the simulation is dust-nudged, and the abstract's 'theoretical predictions' wording overstates the evidential value. The descriptive core of the paper—MEDA pressure records, tide amplitude/phase evolution, image catalog of NPC edge vortices, dust storm kinematics—is well supported and internally consistent for DS-1, DS-A, and DS-C. The phase-response inconsistency for DS-NPC is a genuine but localized correction. I do not see a basis for REJECT: the observed 2–4 sol wave activity and its dusty-season enhancement are directly documented in Figures 2–3, and the model comparison is auxiliary. A CONDITIONAL verdict with requested clarifications therefore remains appropriate; the requested revision should reword 'theoretical predictions' and reconcile the DS-NPC phase statement.","tokens_in":26371,"tokens_out":8235,"duration_ms":82218,"concrete_test":"Rerun the §7.2 LMD PCM experiment for MY36 in free-running mode with climatological dust opacity (no MCS/EMIRS map injection), apply the same 10-sol sliding-window residual analysis at Jezero, and compare periods and amplitudes to Figure 17. If the free run reproduces the dusty-season amplitude increase and 2–4 sol periods, the 'theoretical prediction' claim is supported; if not, the abstract should downgrade the agreement to a dust-forced consistency check.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The paper's headline claim that baroclinic wave activity is 'in good agreement with theoretical predictions by model calculations' rests on the LMD PCM simulation in §7.2. That simulation is not free-running: it uses MY36 MCS- and EMIRS-derived column opacity maps, and dust is injected whenever the simulated column opacity is below the observed map value. The dusty-season growth of simulated 2–4 sol pressure oscillations is thus a radiatively forced response to the observed dust field, not an independent theoretical prediction. A free-running model could still confirm the trend, but the current text overstates the support: the 'agreement' is better described as consistency with a dust-assimilating simulation. A secondary internal inconsistency also needs attention: §6.8 states DS-NPC produced no phase change in sols 650–660, yet the abstract and §8 summary assert that all four dust storms produced inverse tidal phase responses.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper presents a one-Martian-year (MY36 to early MY37) study of atmospheric disturbances at Jezero Crater, combining Perseverance MEDA surface-pressure measurements with orbital imaging from MEX/VMC and MRO/MARCI. It characterizes thermal tides up to the sixth component, long-period (>1 sol) pressure oscillations, dust storms, the Aphelion Cloud Belt, and polar cyclones, and it correlates the seasonal evolution of tidal amplitudes and phases with local aerosol optical depth. The central claims are that the four identified dust storms increased diurnal and semidiurnal tidal amplitudes while producing inverse phase responses, and that the dominant 2-4 sol pressure oscillations are baroclinic in origin, with amplitudes that increase with dust content and with periods and amplitudes in good agreement with LMD Martian PCM simulations. A supporting survey of polar-cap-edge cyclones suggests that some of the observed pressure oscillations may be linked to distant cyclonic vortices.","tokens_in":26540,"tokens_out":4874,"duration_ms":48010,"significance":"If the results hold, the paper provides a valuable multi-instrument, full-season record of Martian synoptic and planetary-scale disturbances at a single site, extending earlier work (Paper 1) to a complete Martian year and adding higher-order tidal components (S1-S6). The descriptive catalog of polar cyclones, dust storms, and their apparent pressure signatures is a useful reference for future comparative studies with other landers. The paper's strengths include the use of established, publicly available pressure-reduction methods, the explicit comparison with MCD and MarsWRF tidal predictions, and the openly available datasets. However, the claim of 'good agreement with theoretical predictions' is weakened by the fact that the PCM simulation is constrained with observed MY36 dust opacity maps rather than being a free-running prediction, and there is an internal inconsistency regarding whether all four dust storms produced inverse tidal phase responses.","major_comments":[{"comment":"The statement that the observed 2-4 sol baroclinic wave activity is 'in good agreement with theoretical predictions by model calculations' is overstated. The PCM simulation described in §7.2 is not free-running: it is constrained by MCS- and EMIRS-derived MY36 column opacity maps, and dust is injected whenever the simulated column opacity falls below the observed map value. The simulated growth of wave amplitudes during the dusty season is therefore a radiatively forced response to the observed dust forcing, not an independent theoretical prediction. The abstract and Summary should be rephrased to say 'consistent with a dust-assimilating PCM simulation,' or the authors should add a genuinely free-running simulation (or a sensitivity run with climatological dust) to validate the dust-wave trend independently.","section":"§7.2 and Abstract"},{"comment":"There is a direct internal inconsistency about whether all four dust storms produced inverse phase responses. The abstract states that 'Three regional dust storms and one polar storm extending over Jezero produced an increase in the diurnal and semidiurnal amplitudes but resulted in inverse responses in their phases,' and the §8 Summary bullet 'Dust Storms and tides' includes the four storms and states that the semidiurnal phase showed punctual increases during the four storms. However, §6.8 explicitly reports that for DS-NPC 'their phases do not show a change in sols 650-660,' and §6.6 already flagged that 'the case of storm DS-NPC is less obvious.' The abstract and Summary must be revised to exclude DS-NPC from the generalized phase-response statement or to explicitly qualify the exception.","section":"Abstract, §8 Summary, and §6.8"},{"comment":"The Summary states that the polar-cap-edge cyclones 'are most probably behind the pressure oscillations detected at Perseverance,' but the body text in §7.2 only offers this as a possibility, noting that if the oscillation were related to the cyclones, the pressure disturbance would need a radius of action 2-3 times larger than the vortex size. The evidence presented is temporal coincidence and distance (1500-4500 km), with no quantitative lag-correlation or composite analysis tying individual cyclone passages to individual pressure oscillations. This causal attribution is load-bearing for the 'Dust Cyclones' summary claim and should either be softened to a hypothesis or supported by a statistical association test between cyclone events and pressure oscillation timings.","section":"§7.2 and §8 Summary, 'Dust Cyclones' bullet"},{"comment":"The dominant-period claim of 2-4 sols rests on the time separation between consecutive peaks in the detrended pressure series, yielding a mean of 3.8 ± 1.9 sols. This method does not provide a spectral estimate with confidence intervals, and the large scatter makes the 'dominant period' identification fragile. A Lomb-Scargle periodogram or wavelet analysis of the detrended pressure would better support the central period range used to argue for baroclinic waves. If such an analysis is already available from Paper 1's methodology, it should be reported here; otherwise the period distribution should be presented as a descriptive peak-count statistic rather than as a validated dominant period.","section":"§5, Figure 3b"}],"minor_comments":[{"comment":"The linear relation is printed as '1.6 0.3τ +' in the text; this should read '1.6 + 0.3τ' both in the text and in the figure caption.","section":"§7.1, Figure 16"},{"comment":"The sentence 'In general the Martian PCM results reproduce the behavior of the tidal amplitudes reasonably well' is ambiguous because the preceding paragraph compares with the Mars Climate Database and MarsWRF, while the PCM simulation is introduced later in §7.2. Please clarify which model output is shown in Figure 2 and use consistent terminology for MCD, MarsWRF, and PCM.","section":"§4"},{"comment":"The phrase 'two-moment aerosol sizes distributions' should be 'two-moment aerosol size distributions,' and the equation for the baroclinic index is garbled in the typeset text and should be reformatted.","section":"§7.2"},{"comment":"The reference to 'Laboratoire de Météorology Dynamique' should be 'Laboratoire de Météorologie Dynamique.'","section":"References"},{"comment":"The sentence 'This is consistent with the high density cloud detection from Ls ∼ 130°-150° by two different Perseverance instruments by Toledo et al. (2023) and Patel et al. (2023)' would read more clearly as 'consistent with the high-density cloud detections from Ls ∼ 130°-150° reported by Toledo et al. (2023) and Patel et al. (2023).'","section":"§6.4"}],"recommendation":"major_revision","confidential_remarks":"The manuscript is a solid observational extension of the authors' earlier Paper 1, and the descriptive dataset will likely be useful to the Mars atmosphere community. The main obstacles to acceptance are the overstated 'theoretical predictions' claim based on a dust-assimilating simulation and the abstract/summary inconsistency about DS-NPC tidal phase behavior. Both are fixable with rephrasing and, ideally, one additional free-running model test. The period-determination comment is also worth addressing because the central baroclinic-wave claim depends on it. I recommend major revision."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Read this as the definitive Jezero pressure climatology for MY36, but don't buy the 'theoretical predictions' framing in the abstract. The core result is descriptive and solid: one Martian year of MEDA pressure, tides up to S6, the 2-4 sol wave field, and orbital imaging of polar cyclones, the double annular cyclone, the Aphelion Cloud Belt, and four dust storms. The seasonal tide-amplitude versus opacity correlation in the dusty season is convincing, and the amplitude/phase responses to DS-1, DS-A, and DS-C are clearly documented. This extends paper 1 to a full year and adds the simultaneous imaging catalog, which is genuinely new.\n\nThe soft spots are real but manageable. First, the 'good agreement with theoretical predictions' for baroclinic waves is an overstatement. The PCM run in Section 7.2 is nudged with MY36 MCS/EMIRS column opacity maps; dust is injected wherever the simulated opacity falls below the observed map. So the simulated dusty-season amplitude growth is a response to the observed dust forcing, not a free-running prediction. The right phrase is 'consistent with a dust-assimilating simulation,' and the abstract and Section 7.2 should say that. Second, there is an internal inconsistency: Section 6.8 states DS-NPC produced no phase change in sols 650–660, while the abstract and Section 8 say all four dust storms produced inverse phase responses. That contradiction needs to be fixed, not finessed. Third, linking specific polar cyclones thousands of kilometers away to ~1–2 Pa pressure oscillations at Jezero is speculative; the authors hedge with 'could be' and I agree it is plausible, but it is not established. Fourth, the period determination from peak separations is crude, but it is enough to pin the 2–4 sol range, which is the main claim. The tide-opacity mixture percentages in Figure 16 are fitted, not predicted, and the paper does not claim otherwise—worth flagging but not a flaw.\n\nWho is this for? Mars atmospheric scientists, rover payload teams, and anyone building a comparative pressure record across InSight, Curiosity, and Zhurong. It deserves a serious referee; the observations are high quality and the dataset is a reference for MY36. My recommendation: accept after minor-to-moderate revision, with the model-language fix and the DS-NPC reconciliation as required changes.","headline":"Solid full-year Jezero pressure climatology; the 'model agreement' claim overstates support because the GCM run is dust-nudged.","tokens_in":27185,"tokens_out":2356,"would_cite":true,"duration_ms":22833,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"A year of Perseverance pressure data and orbiting images shows that Mars's 2-4 sol weather waves are baroclinic disturbances that grow with dust, and that regional dust storms double the daily pressure tides while shifting their phases in…","keywords":["Mars","Perseverance rover","surface pressure","thermal tides","baroclinic waves","dust storms","Jezero Crater","Martian Year 36"],"falsifier":"A decisive test would be to run the same Mars global climate model without prescribing the observed Martian Year 36 dust opacity, using climatological dust instead, and check whether the 2-4 sol pressure oscillations still grow by a factor of two to four during the dusty season; if they do not, the reported agreement is an artifact of the dust forcing. A complementary check would compare Jezero pressure with the simultaneous pressure records at Gale, InSight, and Zhurong to verify that the 2-4 sol oscillations are coherent traveling waves with wavenumbers 1-3 rather than local noise.","tokens_in":26209,"feed_emoji":"🌪️","tokens_out":10758,"duration_ms":94635,"temperature":0.7,"pith_summary":"Using one full Martian year of surface-pressure measurements from Perseverance at Jezero Crater alongside daily global images from two Mars orbiters, this paper identifies which large-scale atmospheric disturbances actually shape the rover's pressure record. It argues that the recurring 2-4 sol pressure oscillations, with amplitudes of about 1-15 Pa, are baroclinic weather waves generated near the edge of the North Polar Cap, and that their amplitude grows with the amount of dust suspended in the atmosphere. It also shows that four dust storms passing near Jezero doubled the diurnal and semidiurnal tidal amplitudes while driving their phases in opposite directions. A sympathetic reader would care because it demonstrates that a single surface station, combined with orbital imagery, can track the planet's dominant weather systems and that the dust cycle is the main switch for both wave and tidal activity.","feed_headline":"Dust storms double Mars pressure tides, Perseverance finds","feed_subtitle":"One full Martian year of rover pressure plus orbiter images ties 2-4 sol waves to dust and high-latitude cyclones.","key_machinery":"The analysis rests on two linked tools. The first is the decomposition of the rover's pressure time series into six thermal-tide components, with periods of 24, 12, 8, 6, 4.8, and 4 hours, plus residual long-period oscillations obtained by subtracting the daily mean and seasonal trend. The second is baroclinic instability theory, quantified through the baroclinic index, the standard growth-rate estimate for weather disturbances powered by horizontal temperature contrasts; the paper evaluates it using climatological wind and temperature profiles near 60°N. Orbital images provide the spatial counterpart, showing polar-edge dust cyclones, the double annular cyclone, and the Aphelion Cloud Belt at known distances from Jezero. A Mars global climate model simulation, forced with that year's observed dust opacity maps, is the quantitative check connecting the dust cycle to the seasonal growth of wave amplitude.","core_discovery":"The paper's central claim is that Jezero's pressure record over Martian Year 36 splits cleanly into two dynamical regimes governed by dust. In the clear first half of the year, long-period pressure oscillations have small peak-to-peak amplitudes, averaging about 1.6 Pa. In the dusty second half they average about 4.2 Pa with peaks above 18 Pa, and the largest event, regional dust storm C, produced an oscillation of about 22 Pa just before the local dust maximum. The paper identifies these 2-4 sol oscillations as baroclinic waves from the northern hemisphere, compatible with the arc-shaped, spiral, and ring-like cyclones seen at the North Polar Cap edge in orbital images, and reports that a Mars global climate model run with the observed year's dust field reproduces the seasonal trend in amplitude and period. For the thermal tides, the diurnal and semidiurnal amplitudes rose by roughly a factor of two during each of the four dust storms, while the diurnal phase fell and the semidiurnal phase rose, a pattern the paper notes agrees with the response recorded at the Viking landers.","pith_inferences":["The climate-model agreement is not a free prediction, because the model is constrained with the observed dust opacity maps; a fairer test of the baroclinic interpretation would rerun the model with climatological dust and see whether the wave amplitude still grows.","If a polar-edge cyclone's pressure influence really extends two to three times beyond its visible dust and cloud size, then simultaneous pressure records at Jezero, Gale, InSight, and Zhurong during this same year could map high-latitude storm passages that imaging alone cannot track.","The full-day phase reversal during dust storm C, occurring before the local opacity maximum, suggests the tide reacts to the horizontal spread of dust over thousands of kilometres rather than just the local column; that could make tide phase a remote gauge of dust-storm extent.","The empirical tide-opacity combination (roughly half diurnal, half semidiurnal, with small contributions from higher components) is fit to one year at one site; checking whether the same weights hold in other years and at other landers would show whether it is a general Martian relation or a local seasonal accident."],"forward_implications":["Dust loading is the main seasonal switch: long-period wave amplitudes at Jezero grow from an average of 1.6 Pa in the clear season to 4.2 Pa in the dusty season, with peaks above 18 Pa.","Regional dust storms act on the tides in a stereotyped way, raising diurnal and semidiurnal amplitudes by roughly a factor of two (10-20 Pa) while the diurnal phase drops and the semidiurnal phase rises.","The 2-4 sol pressure oscillations are the surface expression of baroclinic waves generated near the North Polar Cap edge, so a rover at 18°N can sense high-latitude weather systems from 1,500 to 4,500 km away.","Tide amplitudes track optical depth only during the dusty half-year; in the aphelion cloud belt the diurnal and semidiurnal components follow opposing trends tied to water-ice clouds.","Tidal phase changes can begin 1-3 sols before the local dust opacity peaks, so pressure tides may act as an early indicator of approaching dust storms."],"supporting_citations":[{"why":"Establishes the pressure and tidal analysis methodology and covers the first half of the same Jezero dataset.","marker":"Sánchez-Lavega et al., 2023 (paper 1)"},{"why":"Supplies the Mars general circulation model used for the wave simulations.","marker":"Forget et al., 1999"},{"why":"Supplies the method for generating simulated pressure oscillations and the climate reference data used in the comparison.","marker":"Lewis et al., 1999"},{"why":"Provides the Martian Year 36 column dust opacity maps that constrain the dust field in the simulation.","marker":"Montabone et al., 2023"},{"why":"Gives the baroclinic index used to estimate growth times of the northern-hemisphere disturbances.","marker":"Lindzen & Farrell, 1980"},{"why":"Provides prior orbital evidence for northern-hemisphere baroclinic waves that the observed cyclones are compared with.","marker":"Hinson & Wilson, 2021"},{"why":"Supports the interpretation of 2-5 sol, wavenumber 1-3 waves traveling between Gale and Jezero.","marker":"Battalio et al., 2022"},{"why":"Describes the MEDA instrument and the first 250 sols of Jezero meteorology, the observational basis for this paper.","marker":"Rodríguez-Manfredi et al., 2023"}],"fun_headline_variants":["Mars dust storms boost tidal pressure swings, rover data shows","Perseverance pressure data ties dust storms to larger waves","Jezero's pressure record reveals dust-driven tide shifts","Mars year of pressure data links dust to 2-4 sol waves","Rover and orbiters show Mars dust storms alter pressure tides"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The load-bearing premise is that the climate-model simulation is a fair test of the wave behavior even though its dust field is inserted from observed opacity maps whenever the simulated dust is too low; if the dust forcing, rather than the atmosphere's intrinsic baroclinic response, is what produces the agreement, the validation claim weakens.","fun_headline_variants_meta":{"raw":{"variants":["Mars dust storms boost tidal pressure swings, rover data shows","Perseverance pressure data ties dust storms to larger waves","Jezero's pressure record reveals dust-driven tide shifts","Mars year of pressure data links dust to 2-4 sol waves","Rover and orbiters show Mars dust storms alter pressure tides"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000924,"raw_usage":{"total_tokens":4025,"prompt_tokens":1077,"completion_tokens":2948,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":693,"completion_tokens_details":{"reasoning_tokens":2863}},"tokens_in":693,"tokens_out":2948,"duration_ms":22301,"temperature":1.0,"reasoning_tokens":2863,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-10T21:12:08.037793+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"A decisive test would be to run the same Mars global climate model without prescribing the observed Martian Year 36 dust opacity, using climatological dust instead, and check whether the 2-4 sol pressure oscillations still grow by a factor of two to four during the dusty season; if they do not, the reported agreement is an artifact of the dust forcing. A complementary check would compare Jezero pressure with the simultaneous pressure records at Gale, InSight, and Zhurong to verify that the 2-4 sol oscillations are coherent traveling waves with wavenumbers 1-3 rather than local noise.","supporting_citations":[],"review_version":1}