Pith. sign in

REVIEW 3 major objections 4 minor 45 references

A study on the contribution of the interplanetary medium in radio occultation experiments

T0 review · 3 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Across five spacecraft datasets, the paper isolates and quantifies the interplanetary medium's contribution to Doppler frequency fluctuations, reporting mHz-level amplitudes that set a plasma-noise floor for precision radio tracking.

desk verdict Useful empirical inventory of IPM-induced Doppler noise across five radio links, but the IPM attribution rests on detrending assumptions and single events. read the letter →

arxiv 2608.03435 v1 pith:HZUVPAQD submitted 2026-08-04 astro-ph.EP astro-ph.SRphysics.space-ph

Keshav Aggarwal , R. K. Choudhary , Abhirup Datta , Soumyaneal Banerjee , R. Manikantan , Anshuman Sharma , Takeshi Imamura This is my paper · ORCID
classification astro-ph.EPastro-ph.SRphysics.space-ph
keywords radiooccultationinterplanetarymediumDopplerresidualsplasmaturbulenceChandrayaan-3VenusExpressAkatsukisolarwind
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper tries to establish that the weak, millihertz-level Doppler fluctuations seen in spacecraft radio signals can be attributed to electron-density irregularities in the interplanetary medium, and that those fluctuations are a measurable plasma-noise floor for radio occultation and precision tracking. It does this by selecting five datasets whose line-of-sight geometries keep the signal away from the Moon, planetary atmospheres, and the solar corona (except for two control cases), then analysing Doppler residuals and their power spectra. The paper reports amplitudes of about ±0.01 Hz for S-band over a roughly 35,000 km Earth–Moon path, about ±2.5 Hz for S-band over a 0.91 AU Earth–Venus path, and about ±0.05 Hz for X-band over a 0.29 AU path. If these numbers are right, future missions can budget for interplanetary plasma as a source of Doppler noise that depends on frequency, link configuration, and propagation geometry.

What carries the argument

The central object is the Doppler residual $\Delta f(t)=f_{\mathrm{obs}}(t)-f_{\mathrm{th}}(t)$, defined in Equation (1) as the cumulative refractive effect of plasma irregularities along the two-way propagation path. After detrending the raw residuals with a low-order polynomial or spline, the paper computes power spectral densities of the detrended time series and compares them with a white-noise baseline; departure from a flat spectrum indicates structured, frequency-dependent plasma fluctuations. The two-way coherent link matters because the signal traverses the same plasma twice, so plasma-induced phase perturbations add while many instrumental noise sources cancel.

What would settle it

A definitive check would be a dual-frequency (S-band and X-band) occultation pass along an IPM-only line of sight. Because plasma-induced Doppler shifts scale as $1/f^2$, the S-band and X-band residuals should differ by a factor of roughly $(8.4/2.3)^2\approx 13.3$ if both are dominated by the same IPM irregularities; non-dispersive errors such as spacecraft dynamics or clock drift would appear equally in both bands and break that ratio. If the observed ratio does not hold, the residuals are not purely interplanetary plasma.

Watch

Extended reading notes

Core claim

The paper's central claim is that the Doppler residual $\Delta f(t)=f_{\mathrm{obs}}(t)-f_{\mathrm{th}}(t)$ — the difference between the received spacecraft carrier frequency and a prediction from a relativistic light-time model — is, when the line of sight avoids the Moon, planets, and the Sun, a measurement of electron-density irregularities in the interplanetary medium. After detrending, the residuals show fluctuations of about $\pm 0.01$ Hz for Chandrayaan-3 S-band over an Earth–Moon path of roughly 35,000 km, about $\pm 2.5$ Hz for Venus Express S-band over a 0.91 AU Earth–Venus path, and about $\pm 0.05$ Hz for Akatsuki X-band over a 0.29 AU path. The paper argues that these amplitudes are the interplanetary medium's quantitative contribution to Doppler noise, while the larger values from Chandrayaan-2 lunar occultation ($\pm 0.075$ Hz, spectral index $\alpha\approx 2.18$) and Akatsuki solar occultation ($\pm 2$ Hz, $\alpha\approx 0.68$) bracket the non-IPM plasma environments.

Load-bearing premise

The load-bearing premise is that the detrended Doppler residual is dominated by interplanetary plasma fluctuations rather than by unmodeled spacecraft dynamics, thermal noise, clock drift, or ground-station systematics.

Editorial extensions

If this is right

  • Interplanetary plasma alone produces Doppler fluctuations of about $\pm 0.01$ Hz at S-band over a ~35,000 km Earth–Moon path, far smaller than the ~$\pm 0.075$ Hz seen when the same two-way S-band link passes through the lunar ionosphere.
  • At X-band over a 0.29 AU Earth–Venus path, IPM-only fluctuations are about $\pm 0.05$ Hz, while the same link at 3.9 solar radii shows $\pm 2$ Hz, so coronal plasma dominates by roughly two orders of magnitude.
  • Two-way coherent S-band links are more sensitive to weak IPM fluctuations than one-way X-band links, because the two-way geometry doubles the plasma phase accumulation while cancelling many instrumental noise sources.
  • Power spectral slopes separate environments: near-lunar and coronal occultation spectra show power-law behavior consistent with an inertial-range cascade, while IPM-only spectra are nearly flat or slightly negative, indicating weak, low-amplitude turbulence far from the Sun and Moon.
  • The absence of a measurable Doppler-spectrum response to a solar flare in the Chandrayaan-3 data suggests that not every transient solar event produces sufficient plasma along the line of sight to alter the observed fluctuations.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Inference: A dual-frequency version of the same experiment would test the IPM attribution directly, since a $1/f^2$ plasma signature would force S-band and X-band residuals into a ratio of roughly $(8.4/2.3)^2\approx 13.3$, while non-dispersive errors would not scale that way.
  • Inference: Applying the same detrending and spectral pipeline to archival tracking data from other deep-space missions could turn these single-pass case studies into a statistical map of how IPM turbulence strength varies with heliocentric distance, solar cycle, and line-of-sight length.
  • Inference: Because the Doppler residual is a path-integrated measurement, the technique could be extended beyond noise characterization: with independent electron-density priors, the residuals could be inverted for line-of-sight integrated electron-content fluctuations, offering a remote plasma diagnostic in regions where in-situ spacecraft coverage is sparse.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper analyzes Doppler residuals from five radio occultation datasets: two-way S-band from the Chandrayaan-3 propulsion module (CH3PM) outside the lunar ionosphere, two-way S-band from Chandrayaan-2 (CH2) in lunar occultation, one-way S-band from Venus Express (VeRa) in IPM-only geometry, one-way X-band from Akatsuki in IPM-only geometry, and one-way X-band from Akatsuki in solar occultation. The authors compute residuals Δf = f_obs − f_th using a relativistic light-time model, detrend them with polynomials or splines, and attribute the detrended fluctuations to the interplanetary medium (IPM). They report mHz-level fluctuations for IPM-only datasets, larger fluctuations for CH2 and solar occultation, and power spectral density spectral indices ranging from −0.68 to 2.18. The central claim is that these results quantify the IPM contribution to Doppler noise and demonstrate the enhanced plasma sensitivity of two-way coherent S-band links.

Significance. If the attribution of the detrended residuals to IPM is valid, the paper provides useful multi-frequency empirical constraints on IPM turbulence far from the Sun and a benchmark for plasma-induced noise in spacecraft tracking and radio science. The study covers a useful spread of frequencies, link configurations, and geometries, and the CH3PM two-way S-band detection of mHz-level fluctuations is a potentially interesting result. However, the quantitative claims currently rest on an untested assumption that the residuals are plasma-dominated; the paper does not provide a dispersive discriminator, and the spectral analysis contains internal inconsistencies and no uncertainties. The significance of the paper depends on resolving these issues.

major comments (3)
  1. [Section 3.5, Table 1, Abstract] The manuscript contains a direct contradiction about the CH2 spectral index. In Section 3.5 it states that CH2 has α ~ 2.18, 'which implies steep, non-Kolmogorov, dissipative turbulence,' and later in the same section that 'The CH2 S-band and Akatsuki X-band solar occultation datasets exhibit clear power-law behavior over a broad frequency range, with slopes consistent with Kolmogorov turbulence.' The abstract's claim of Kolmogorov-like turbulence for the lunar occultation case is inconsistent with the reported α = 2.18. Please correct this discrepancy and specify the expected Kolmogorov value (α = 2/3).
  2. [Section 2.1, Eq. (1), Sections 3.1–3.3] The central attribution of the detrended Doppler residuals to IPM is not validated. Equation (1) defines Δf(t) as the cumulative refractive effect of plasma, but this is an interpretive assumption: the residual also contains any unmodeled dynamics, oscillator noise, ground-station systematics, and media other than the IPM. The paper does not perform a dispersive test (for plasma, simultaneous S/X amplitude ratio near f_X/f_S and high correlation; for non-dispersive systematics, ratio near unity), nor does it report an Allan-deviation or calibration pass. For the one-way VeRa S-band pass, where the raw drift is about 1000 Hz over 90 minutes and a spline removes it, the remaining ±2.5 Hz could equally be produced by a slow frequency offset or unmodeled spacecraft motion. For CH3PM, unmodeled non-gravitational accelerations in a highly elliptical orbit could leave mHz-level residuals after polynomial detrending. Unless a dispersive check is provided or the claims are explicitly downgraded to upper limits or interpretation, the abstract's 'quantify' statement is not supported.
  3. [Section 3.5, Table 1, Figures 5–9] The spectral slopes are reported without uncertainties and without a sensitivity analysis. The detrending order/type (second-order polynomial for CH3PM, spline for VeRa) is chosen per dataset and can suppress genuine low-frequency signal or introduce spurious spectral slopes. The fit range [1/N, f_N/10] is stated, but no fitting method or confidence intervals are given. The interpretation of negative α as 'no discernible information' is then contradicted by the later claim that the same datasets 'reflect weak interplanetary turbulence.' Please provide slope uncertainties, a detrending-order sensitivity test, and a clear criterion for when a spectral index is physically meaningful.
minor comments (4)
  1. [References] Aggarwal et al. 2026a and 2026b appear with identical titles and DOIs; please merge or distinguish them.
  2. [Abstract] The phrase 'one-way S/X band measurements from the Venus Express Radio Science (VeRa)/Akatsuki' is ambiguous: Section 2.3 describes VeRa as S-band only. Please clarify that S-band is from VeRa and X-band from Akatsuki.
  3. [Table 1 and text] The statement that all observations correspond to 'quiet solar and geomagnetic conditions, as indicated by the daily averaged Dst values' is at odds with the reported Dst = 50 for CH2 and the description of X-class flares and CMEs during the CH3PM interval in Sections 1 and 2.1. Please reconcile the text with the Table entries.
  4. [Figure 10, Section 3.4] The white-noise comparison is only qualitative; no statistical test (e.g., confidence bands on the PSD) is used to establish that the observed PSDs are significantly non-flat.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the IPM attribution is an empirical residual interpretation, not a fitted prediction or a self-citation reduction.

full rationale

The paper is an empirical, multi-dataset radio-occultation analysis rather than a derivation whose conclusion is folded into its inputs. Equation (1) defines the Doppler residual as Δf(t) = f_obs(t) − f_th(t), which is an identity; the subsequent statement that the residual 'represent[s] the cumulative refractive effects of plasma irregularities' is an interpretive attribution based on the selected observing geometries, not a quantity constructed from plasma parameters. No fitted parameter is later renamed as the reported IPM fluctuation amplitude: the detrending polynomials and splines are data-conditioning steps, and the reported mHz-level fluctuations are the remaining residuals, not predictions generated from a fitted model. The spectral-slope interpretation uses an external Kolmogorov benchmark (α = 2/3 via p = 11/3), so it is not self-referential. The self-citations present (e.g., Aggarwal et al. 2026a for polynomial detrending and Aggarwal et al. 2025a,b, 2026a,b for coronal/IPM context) are not load-bearing: the same methodological choices are also supported by external references (Wexler et al. 2019; Gramigna et al. 2023), and the central measurements come from independent spacecraft data. The paper also explicitly limits its claims, noting that the analyzed solar flare produced no measurable Doppler spectral-slope change and that a larger statistical database is needed, which confirms that the conclusions are empirical and falsifiable rather than definitional. I therefore find no circular step that reduces the central claim to its own inputs.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central claims rest mainly on geometry-based isolation of the IPM and on detrended Doppler residuals. The detrending coefficients and PSD slopes are fitted quantities, but no new physical free parameters are introduced and no new entities are postulated.

free parameters (2)
  • Per-dataset detrending function coefficients = not reported
    Second-order polynomial (CH3PM), spline (VeRa), and polynomial (Akatsuki) fits absorb slow variations; the residual is treated entirely as the IPM signal, so the central amplitude claim depends on these fitted curves.
  • PSD spectral slope alpha = -0.68 (CH3PM), 0.01 (VeRa), -0.28 (Akatsuki IPM), 0.68 (solar occultation), 2.18 (CH2)
    Fitted over the range [1/N, f_N/10] and used to classify turbulence as Kolmogorov-like or not; no uncertainties are reported.
assumptions (5)
  • standard math Cold plasma refractive index scales as 1/f^2, so lower-frequency S-band signals are more plasma-sensitive than X-band.
    Invoked in Section 1 to interpret the frequency dependence of the observed Doppler fluctuations.
  • domain assumption Two-way coherent links traverse the same plasma path twice, doubling plasma phase perturbations while canceling many instrumental noise sources.
    Stated in Section 1 and used to explain the higher sensitivity of CH2 and CH3PM measurements.
  • ad hoc to paper The detrended Doppler residual is dominated by plasma effects along the line of sight.
    Introduced in Sections 3.1 to 3.3; no independent validation is provided against unmodeled spacecraft dynamics or ground systematics.
  • standard math Kolmogorov turbulence maps to a PSD slope alpha = p - 3 = 2/3.
    Used in Section 3.5 to interpret the fitted spectral slopes as signatures of turbulence.
  • domain assumption The CH3PM line of sight at 30,000 to 90,000 km from the lunar center avoids the lunar ionosphere.
    Required to isolate the IPM contribution from near-lunar plasma; the lunar ionosphere is assumed negligible at these distances.

how reviews work

0 comments
Cite this review

Pith. "Pith review of A study on the contribution of the interplanetary medium in radio occultation experiments." pith.science (2026). https://pith.science/paper/HZUVPAQD

@misc{pith2026260803435,
  author       = {Pith},
  title        = {Pith review of: A study on the contribution of the interplanetary medium in radio occultation experiments},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HZUVPAQD}},
  note         = {Machine review of arXiv:2608.03435}
}
read the original abstract

Irregularities in electron density within the interplanetary medium (IPM) can cause fluctuations in the Doppler frequency of spacecraft radio signals. The amplitude of these fluctuations depends on factors such as the carrier frequency, propagation geometry, and link configuration. However, quantitative characterization of these effects across different frequencies in various occultation experiments is currently limited. We analyze five complementary datasets: two-way S-band observations from Chandrayaan-3 outside the lunar ionosphere, two-way S-band data from Chandrayaan-2 during lunar occultation, one-way S/X band measurements from the Venus Express Radio Science (VeRa)/Akatsuki Radio Science (Akatsuki) under IPM-only conditions, and one-way X-band Akatsuki data during solar occultation. The Chandrayaan-3 and Akatsuki IPM observations isolate IPM effects by excluding contributions from planetary atmospheres, the lunar ionosphere, and, except during solar occultation, the solar corona. Chandrayaan-3 data sample dynamically evolving Earth-Moon geometries and exhibit weak, mHz-level Doppler fluctuations, while Chandrayaan-2 observations provide near-lunar plasma benchmarks with higher amplitudes, during quiet time solar and geomagnetic conditions. Akatsuki and VeRa's IPM-only measurements capture long-path interplanetary effects, whereas Akatsuki solar occultation data reveal strong coronal signatures. Power spectral density analysis indicates Kolmogorov-like turbulence for lunar occultation and solar occultation cases, while IPM-only spectra show low-amplitude fluctuations. These results quantify the IPM contribution to Doppler noise, demonstrate the enhanced plasma sensitivity of two-way coherent links, and provide constraints relevant to turbulence modelling, precision spacecraft tracking, and the interpretation of radio occultation experiments.

Figures

Figures reproduced from arXiv: 2608.03435 by the authors.

Figure 1
Figure 1. Positions of the CH3PM propulsion module during DOY 313–320 2025. Blue curve: spacecraft trajectory; colored points: positions; [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Left Panel: Position of the Moon (point in grey) and CH3PM (point in black) on 10 November 2025 (DOY 314) 2025. Right panel: Position of the Moon/CH2 orbiter on 08 November 2022 (DOY 312, black) against the position of Earth (blue point). This configuration allows Doppler residuals to include contributions from lunar ionosphere and near-lunar plasma. Theoretical magnetopause boundaries are shown in red and blue, and… view at source ↗
Figure 3
Figure 3. Observing geometry for VeRa S-band measurements on 15 [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Observing geometry for Akatsuki X-band measurements. Left: Maximum LOS separation from the Sun on 08 June 2020 (IPM-only). [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]
Figure 5
Figure 5. Figure 5: CH3PM S-band observations for DOY 314, 10 November 2025. Top left: raw Doppler residuals (blue) with trend fit (orange). Bottom [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 6
Figure 6. Figure 6: CH2 S-band Doppler residuals (DOY 312, 08 November 2022). Top left: raw Doppler residuals (blue) with composite fit (orange). [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: VeRa S-band IPM-only residuals (15 Dec 2008). Top left: raw residuals (blue) with trend (orange). Bottom left: detrended residuals [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 8
Figure 8. Figure 8: Akatsuki X-band IPM-only residuals (08 June 2020). Top left: raw residuals (blue) with trend (orange). Bottom left: detrended residuals [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]
Figure 9
Figure 9. Figure 9: Akatsuki X-band residuals during solar occultation (23 October 2022, 3.9 [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]
Figure 10
Figure 10. Figure 10: Top Panel: Pure white noise generated using Python, with [PITH_FULL_IMAGE:figures/full_fig_p011_10.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

45 extracted references · 21 canonical work pages

  1. [1]

    , year 1996

    author Acton, C.H. , year 1996 . title Ancillary data services of nasa's navigation and ancillary information facility . journal Planetary and Space Science volume 44 , pages 65--70 . :10.1016/0032-0633(95)00107-7

    doi:10.1016/0032-0633(95)00107-7 1996

  2. [3]

    , author Choudhary, R.K

    author Aggarwal, K. , author Choudhary, R.K. , author Datta, A. , author Banerjee, S. , author Imamura, T. , author Ando, H. , year 2026 b. title A turbulence index independent framework for deriving solar wind speed and coronal electron density from radio spectral broadening . journal Monthly Notices of the Royal Astronomical Society volume 548 . http://...

    work page doi:10.1093/mnras/stag554 2026

  3. [4]

    , author Choudhary, R.K

    author Aggarwal, K. , author Choudhary, R.K. , author Datta, A. , author Imamura, T. , year 2025 a. title On the estimation of solar wind velocity under varying solar activity conditions using akatsuki measurements . journal Monthly Notices of the Royal Astronomical Society :10.1093/mnras/staf1305

    work page doi:10.1093/mnras/staf1305 2025

  4. [5]

    , author Choudhary, R.K

    author Aggarwal, K. , author Choudhary, R.K. , author Datta, A. , author Roopa, M.V. , author Dai, B.K. , year 2025 b. title Insights into solar wind flow speeds from the coronal radio occultation experiment: Findings from the indian mars orbiter mission . journal The Astrophysical Journal volume 982 . :10.3847/1538-4357/adb627

    work page doi:10.3847/1538-4357/adb627 2025

  5. [6]

    , author Shiota, D

    author Ando, H. , author Shiota, D. , author Imamura, T. , author Tokumaru, M. , author Asai, A. , author Isobe, H. , author Päzold, M. , author Häusler, B. , author Nakamura, M. , year 2015 . title Internal structure of a coronal mass ejection revealed by akatsuki radio occultation observations . journal journal of Geophysical Research: Space Physics vol...

    doi:10.1002/2015ja021076 2015

  6. [7]

    , author Pearson, B

    author Annex, A. , author Pearson, B. , author Seignovert, B. , author Carcich, B. , author Eichhorn, H. , author Mapel, J. , author von Forstner, J. , author McAuliffe, J. , author del Rio, J. , author Berry, K. , author Aye, K.M. , author Stefko, M. , author de Val-Borro, M. , author Kulumani, S. , author Murakami, S.y. , year 2020 . title Spiceypy: a p...

    doi:10.21105/joss.02050 2020

  7. [8]

    , author Efimov, A

    author Armand, N. , author Efimov, A. , author Samoznaev, L. , author Bird, M. , author Edenhofer, P. , author Plettemeier, D. , author Wohlmuth, R. , year 2003 . title The spectra and cross correlation of radio wave frequency fluctuations observed during coronal plasma sounding with spacecraft signals . journal Journal of Communications Technology and El...

    work page 2003

  8. [9]

    , author Woo, R

    author Armstrong, J.W. , author Woo, R. , author Armstrong, J.W. , author Woo, R. , year 1981 . title Solar wind motion within 30 r solar masses - spacecraft radio scintillation observations . journal A&A volume 103 , pages 415--421 . ui.adsabs.harvard.edu/abs/1981A&A...103..415A

    work page 1981

Show all 45 references
  1. [10]

    , author Riley, P

    author Badman, S.T. , author Riley, P. , author Jones, S.I. , author Kim, T.K. , author Allen, R.C. , author Arge, C.N. , author Bale, S.D. , author Henney, C.J. , author Kasper, J.C. , author Mostafavi, P. , et al., year 2023 . title Prediction and verification of parker sola...

    2023

  2. [11]

    , year 1982

    author Bird, M.K. , year 1982 . title Coronal investigations with occulted spacecraft signals . journal Space Science Reviews 1982 33:1 volume 33 , pages 99--126 . :10.1007/BF00213250

    1982 doi

  3. [12]

    , year 2002

    author Chao, J.K. , year 2002 . title Models for the size and shape of the earth's magnetopause and bow shock . publisher Elsevier . chapter chapter 8 . p. pages 127–135 . :10.1016/s0964-2749(02)80212-8

    2002 doi

  4. [13]

    , author Harmon, J

    author Coles, W. , author Harmon, J. , year 1989 . title Propagation Observations of the Solar Wind near the Sun . journal Astrophysical Journal volume 337 , pages 1023 . :10.1086/167173

    1989 doi

  5. [14]

    , year 1978

    author Coles, W.A. , year 1978 . title Interplanetary scintillation . journal Space Science Reviews volume 21 , pages 411--425 . :10.1007/BF00173067

    1978 doi

  6. [15]

    , author Liu, W

    author Coles, W.A. , author Liu, W. , author Harmon, J.K. , author Martin, C.L. , year 1991 . title The solar wind density spectrum near the sun: Results from voyager radio measurements . journal journal of Geophysical Research: Space Physics volume 96 , pages 1745--1755 . :10...

    1991 doi

  7. [16]

    , author Armand , N.A

    author Efimov , A.I. , author Armand , N.A. , author Samoznaev , L.N. , author Bird , M.K. , author Chashei , I.V. , author Edenhofer , P. , author Plettemeier , D. , author Wohlmuth , R. , year 2003 . title Characteristics of the Near-Sun Solar Wind Turbulence from Spacecraft...

    2003 doi

  8. [17]

    , author Chashei, I.V

    author Efimov, A.I. , author Chashei, I.V. , author Samoznaev, L.N. , author Andreev, V.E. , author Bird, M.K. , author Edenhofer, P. , author Plettemeier, D. , author Wohlmuth, R. , year 2002 . title The outer scale of solar-wind turbulence from galileo coronal-sounding data ...

    2002 doi

  9. [18]

    , author Chasheǐ, I.V

    author Efimov, A.I. , author Chasheǐ, I.V. , author Bird, M.K. , author Samoznaev, L.N. , author Plettemeier, D. , year 2005 . title Turbulence in the inner solar wind determined from frequency fluctuations of the downlink signals from the ulysses and galileo spacecraft . jour...

    2005 doi

  10. [19]

    , author Imamura, T

    author Efimov, A.I. , author Imamura, T. , author Oyama, K.I. , author Noguchi, K. , author Samoznaev, L.N. , author Nabatov, A.S. , author Bird, M.K. , author Chashei, I.V. , year 2010 . title Properties of solar wind turbulence from radio occultation experiments with the noz...

    2010 doi

  11. [20]

    , author Kliore, A.J

    author Fjeldbo, G. , author Kliore, A.J. , author Eshleman, V.R. , year 1971 . title The neutral atmosphere of venus as studied with the mariner v radio occultation experiments . journal The Astronomical Journal volume 76 , pages 123 . :10.1086/111096

    1971 doi

  12. [21]

    , author Parisi, M

    author Gramigna, E. , author Parisi, M. , author Buccino, D. , author Casajus, L.G. , author Zannoni, M. , author Bourgoin, A. , author Tortora, P. , author Oudrhiri, K. , year 2023 . title Analysis of nasa's dsn venus express radio occultation data for year 2014 . journal Adv...

    2023 doi

  13. [22]

    , author Bezrukikh, V.V

    author Gringauz, K.I. , author Bezrukikh, V.V. , author Ozerov, V.D. , author Rybchinskii, R.E. , year 1960 . title Investigation of interplanetary ionized gas, high energy electrons and solar corpuscular radiations by means of 3-electrode traps for charge-carrying particles i...

    1960

  14. [23]

    , author Sahraoui, F

    author Hadid, L.Z. , author Sahraoui, F. , author Galtier, S. , author Huang, S. , year 2018 . title Compressible magnetohydrodynamic turbulence in the earth's magnetosheath: Estimation of the energy cascade rate using in situ spacecraft data . journal Physical Review Letters ...

    2018 doi

  15. [24]

    a usler, B. , author P\

    author H\" a usler, B. , author P\" a tzold, M. , author Tyler, G. , author Simpson, R. , author Bird, M. , author Dehant, V. , author Barriot, J.P. , author Eidel, W. , author Mattei, R. , author Remus, S. , author Selle, J. , author Tellmann, S. , author Imamura, T. , year 2...

    2006 doi

  16. [25]

    , author Ando, H

    author Imamura, T. , author Ando, H. , author Tellmann, S. , author Pätzold, M. , author Häusler, B. , author Yamazaki, A. , author Sato, T.M. , author Noguchi, K. , author Futaana, Y. , author Oschlisniok, J. , author Limaye, S. , author Choudhary, R.K. , author Murata, Y. , ...

    2017

  17. [26]

    , author Noguchi, K

    author Imamura, T. , author Noguchi, K. , author Nabatov, A. , author Oyama, K.I. , author Yamamoto, Z. , author Tokumaru, M. , year 2005 . title Phase scintillation observation during coronal sounding experiments with nozomi spacecraft . journal Astronomy and Astrophysics vol...

    2005 doi

  18. [27]

    , author Toda, T

    author Imamura, T. , author Toda, T. , author Tomiki, A. , author Hirahara, D. , author Hayashiyama, T. , author Mochizuki, N. , author ichi Yamamoto, Z. , author Abe, T. , author Iwata, T. , author Noda, H. , author Futaana, Y. , author Ando, H. , author Häusler, B. , author ...

    2011

  19. [28]

    , author Choudhary, R.K

    author Jain, R.N. , author Choudhary, R.K. , author Bhardwaj, A. , author Imamura, T. , author Sharma, A. , author Parikh, U.M. , year 2023 . title Turbulence dynamics and flow speeds in the inner solar corona: results from radio-sounding experiments by the Akatsuki spacecraft...

    2023 doi

  20. [29]

    , author Choudhary, R.K

    author Jain, R.N. , author Choudhary, R.K. , author Imamura, T. , year 2024 . title Exploring the influence of the ‘Smiley Sun’ on the dynamics of inner solar corona and near-Earth space environment . journal Monthly Notices of the Royal Astronomical Society: Letters volume 52...

    2024 doi

  21. [30]

    , author Patel, I.L

    author Kliore, A.J. , author Patel, I.L. , author Woiceshyn, P.M. , author Nagy, A.F. , author Cravens, T.E. , year 1979 . title The ionosphere of venus: Observations and their interpretation . journal Science volume 205 , pages 99--102 . :10.1126/science.205.4401.99. note pio...

    1979 doi

  22. [31]

    , author Nel, A.E

    author Lotz, S. , author Nel, A.E. , author Wicks, R.T. , author Roberts, O.W. , author Engelbrecht, N.E. , author Strauss, R.D. , author Botha, G.J.J. , author Kontar, E.P. , author Pitňa, A. , author Bale, S.D. , year 2023 . title The radial variation of the solar wind turbu...

    2023 doi

  23. [32]

    , author Pogrebenko, S.V

    author Molera Calv\'es, G. , author Pogrebenko, S.V. , author Cimo, G. , author Duev, D.A. , author Bocanegra-Baham\'on, T.M. , author Wagner, J.F. , author Kallunki, J. , author de Vicente, P. , author Kronschnabl, G. , author Haas, R. , author Quick, J. , author Maccaferri, ...

    2014

  24. [33]

    , author Esposito , P.B

    author Muhleman , D.O. , author Esposito , P.B. , author Anderson , J.D. , year 1977 . title The electron density profile of the outer corona and the interplanetary medium from Mariner-6 and Mariner-7 time-delay measurements. journal Astrophysical Journal volume 211 , pages 94...

    1977 doi

  25. [34]

    , author Karl, J

    author Paetzold, M. , author Karl, J. , author Bird, M.K. , author Paetzold, M. , author Karl, J. , author Bird, M.K. , year 1996 . title Coronal radio sounding with ulysses: dual-frequency phase scintillation spectra in coronal holes and streamers. journal A&A volume 316 , pa...

    1996

  26. [35]

    , year 1958

    author Parker , E. , year 1958 . title Dynamics of the Interplanetary Gas and Magnetic Fields. journal ApJ volume 128 , pages 664 . :10.1086/146579

    1958 doi

  27. [36]

    , author Khokhlachev, A.A

    author Rakhmanova, L.S. , author Khokhlachev, A.A. , author Riazantseva, M.O. , author Yermolaev, Y.I. , author Zastenker, G.N. , year 2024 . title Turbulence development behind the bow shock during disturbed and undisturbed solar wind . journal Solar-Terrestrial Physics volum...

    2024

  28. [37]

    , author Narita, Y

    author Roberts, O.W. , author Narita, Y. , author Nakamura, R. , author V\" o r\" o s, Z. , year 2023 . title Spectral break of the density power spectrum in solar wind turbulence . journal Astronomy & Astrophysics volume 677 , pages L16 . :10.1051/0004-6361/202346709

    2023 doi

  29. [38]

    , author Chao, J.K

    author Shue, J. , author Chao, J.K. , author Fu, H.C. , author Russell, C.T. , author Song, P. , author Khurana, K.K. , author Singer, H.J. , year 1997 . title A new functional form to study the solar wind control of the magnetopause size and shape . journal Journal of Geophys...

    1997 doi

  30. [39]

    , author Zong, Q

    author Tian, T. , author Zong, Q. , author Wang, Y. , author Fei, Z. , year 2012 . title Statistical study of the properties of the magnetic field and plasma in the earth’s magnetotail near lunar orbit . journal Science China Technological Sciences volume 55 , pages 2570–2577 ...

    2012 doi

  31. [40]

    , author Chakrabarty, D

    author Tripathi, D. , author Chakrabarty, D. , author Nandi, A. , author Raghvendra Prasad, B. , author Ramaprakash, A.N. , author Shaji, N. , author Sankarasubramanian, K. , author Satheesh Thampi, R. , author Yadav, V.K. , year 2022 a. title The aditya-l1 mission of isro . j...

    2022 doi

  32. [41]

    , author Choudhary, R.K

    author Tripathi, K.R. , author Choudhary, R.K. , author Ambili, K.M. , year 2025 . title Lunar ionosphere in the geotail region as observed by chandrayaan-2 orbiter using two-way radio occultation measurements: Supplementary section . note Doi:10.5281/zenodo.14604842

    2025 doi

  33. [42]

    , author Choudhary, R.K

    author Tripathi, K.R. , author Choudhary, R.K. , author Jayalal, L. , year 2022 b. title On the estimation of frequency residuals in a radio occultation experiment . journal Monthly Notices of the Royal Astronomical Society :10.1093/MNRAS/STAC2653

    2022 doi

  34. [43]

    , author Hollweg, J.V

    author Wexler, D.B. , author Hollweg, J.V. , author Efimov, A.I. , author Song, P. , author Jensen, E.A. , author Lionello, R. , author Vierinen, J. , author Coster, A.J. , year 2019 . title Radio occultation observations of the solar corona over 1.60-1.86 r_ : Faraday rotatio...

    2019 doi

  35. [44]

    , author Kooi, J.E

    author Wexler, D.B. , author Kooi, J.E. , author Jensen, E.A. , author Song, P. , year 2022 . title Slow solar wind acceleration through the middle corona: Spacecraft radio studies . journal Frontiers in Astronomy and Space Sciences volume Volume 9 . :10.3389/fspas.2022.1047875

    2022

  36. [45]

    , year 2009

    author Withers, P. , year 2009 . title A review of observed variability in the dayside ionosphere of mars . journal Advances in Space Research volume 44 , pages 277--307 . :10.1016/j.asr.2009.04.027

    2009 doi

  37. [46]

    , author Armstrong, J.W

    author Woo, R. , author Armstrong, J.W. , year 1979 . title Spacecraft radio scattering observations of the power spectrum of electron density fluctuations in the solar wind . journal journal of Geophysical Research: Space Physics volume 84 , pages 7288--7296 . :10.1029/JA084I...

    1979 doi

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.