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REVIEW 3 major objections 4 minor 34 references

Modelling atmospheric escape and MgII near-ultraviolet absorption of the highly irradiated hot Jupiter WASP-12b

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read Tidal gravity, not a bow shock, drives WASP-12b's escape

desk verdict Despite a solid multi-fluid model application and a physically plausible captured-by-the-star regime, the paper's headline claims about reproducing the MgII ingress are undercut by the model's axisymmetry and a fitted stellar wind density. read the letter →

arxiv 1908.02527 v1 pith:MJXZBGML submitted 2019-08-07 astro-ph.EP

N. K. Dwivedi , M. L. Khodachenko , I. F. Shaikhislamov , L. Fossati , H. Lammer , Y. Sasunov , A. G. Berezutskiy , I. B. Miroshnichenko
show 3 more authors
K. G. Kislyakova C. P. Johnstone M. Güdel
This is my paper · ORCID
classification astro-ph.EP
keywords hotJupiterWASP-12batmosphericescapestellarwindMgIIabsorptionhydrodynamicmodellingRochelobeoverflowearlyingress
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

Using a 2D multi-fluid hydrodynamic model of WASP-12b's hydrogen-dominated upper atmosphere, this paper argues that the planet's escape is controlled by the host star's tidal pull rather than by the stellar wind. When the tidal force is included, even a fast and dense stellar wind cannot stop the planetary outflow; the material instead splits into two streams moving toward and away from the star, with a saturated mass-loss rate near $10^{12}\ \mathrm{g\,s^{-1}}$. That 'captured by the star' regime is presented as the realistic one for WASP-12b, whose Roche lobe is only $1.37\,R_P$. The paper also computes MgII h-line absorption from the simulated outflow and finds 4--10% absorption in the realistic case, with no early ingress, while the previously proposed bow-shock scenario only appears when tidal effects are artificially switched off. If correct, the simulations rule out the bow-shock explanation for the observed variable early ingress and reframe WASP-12b as a planet whose atmosphere is being accreted by its star.

What carries the argument

The load-bearing object is the 2D axisymmetric multi-fluid hydrodynamic model of Shaikhislamov et al. (2014, 2016) and Khodachenko et al. (2015, 2017), applied to WASP-12b with hydrogen ionization/recombination chemistry and minor species He and Mg treated as separate fluids. The crucial knob is the averaged tidal gravitational potential of equation (A.5), which shortens the Roche radius to $R_{L1}=1.37\,R_P$; switching it on or off defines the two scenarios ('captured by the star' versus 'blown by the wind'). Absorption is computed by integrating Voigt-profile optical depth through the simulated MgII density, velocity, and temperature fields, with a resonant double-charge-exchange reaction between MgI and HeII included because it removes MgII near the planet.

What would settle it

Run a 3D simulation of WASP-12b that includes the Coriolis force and lets the stellar wind arrive at an angle to the XUV flux: if the resulting MgII column ahead of the planet shifts the computed transit ingress earlier than the optical contact, the paper's central conclusion of no early ingress in the realistic regime is falsified. The observed variable early ingress in the NUV transit light curves is the corresponding existing test.

Watch

Extended reading notes

Core claim

The central claim is that WASP-12b's upper atmosphere is in a 'captured by the star' escape regime: the stellar gravitational pull extends the planetary wind beyond the Roche lobe and splits it into two streams along the planet-star axis, so the mass-loss rate (saturated at roughly $1{-}2\times10^{12}\ \mathrm{g\,s^{-1}}$) is set by gravity, not by the XUV heating rate or the stellar wind ram pressure. In this regime the stellar wind only compresses the streams laterally and picks up ions near the boundary; it does not stop the outflow. A bow shock ahead of the planet, the configuration previously invoked to explain early NUV ingress, forms only in a test case with no tidal force and a slow, dense wind, which the authors call unrealistic for WASP-12b. Simulated MgII h-line absorption reaches 4--10% in the realistic scenario (larger for rarer winds), and the simulated transit curves in the shock scenario begin at the optical transit, meaning no early ingress is produced; the paper concludes that a complete account of the observed early ingress would require three-dimensional geometry.

Load-bearing premise

The model's 2D axisymmetric geometry ignores the Coriolis force and assumes the stellar wind and XUV flux arrive along the same direction, so the computed MgII distribution is trusted only within about five planetary radii; if Coriolis bending redirects the absorbing stream, the conclusion of no early ingress could change.

Editorial extensions

If this is right

  • WASP-12b's outflow is gravitationally captured by the star, so the planet is likely feeding material into a circumplanetary or circumstellar torus rather than shedding it as a comet-like tail.
  • The mass-loss rate in the realistic regime is 10--15 times higher than in the no-tide case and saturates near $10^{12}\ \mathrm{g\,s^{-1}}$, so evolutionary estimates based on XUV-driven energy-limited escape alone would underestimate the planet's mass loss.
  • Bow-shock interpretations of WASP-12b's variable early NUV ingress are not supported by a self-consistent wind solution; the observed early absorption would need explanation from 3D structure, such as Coriolis bending or a torus of previously escaped material.
  • MgII absorption is more sensitive to stellar wind density than to XUV flux in the captured regime, so NUV MgII transit depth can serve as a probe of the local stellar wind environment around the planet.

Reading between the lines

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

  • If the captured-by-the-star regime is real, WASP-12b is a natural laboratory for star-feeding accretion streams; a 3D simulation with the Coriolis force would predict whether the two streams bend prograde and create the observed variable early ingress by placing MgII ahead of the planet along the orbit.
  • Because the simulated mass-loss rate in the realistic scenario depends only weakly on XUV flux, reconstructing the host star's XUV history from WASP-12b's current escape rate would be unreliable; the escape rate is mostly a gravity diagnostic instead.
  • The same two-scenario test could be applied to other ultra-hot Jupiters near their Roche limit: for planets with larger $R_{L1}/R_P$, the bow-shock regime may become realistic, making the presence of early ingress a diagnostic of orbital distance and stellar wind conditions.
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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 manuscript presents two-dimensional, multi-fluid hydrodynamic simulations of the upper atmosphere of the hot Jupiter WASP-12b, including hydrogen photo-chemistry and minor species Mg and He, under different stellar XUV fluxes and stellar wind conditions. Two interaction regimes are considered: a 'captured by the star' scenario with tidal force and a fast stellar wind, and a 'blown by the wind' scenario without tidal force and a slow wind. The authors compute MgII h-line absorption and compare it with HST/COS near-ultraviolet observations, reporting that the captured-by-the-star scenario produces two streams and a mass-loss rate of about 10^12 g/s but no early ingress, whereas the blown-by-the-wind scenario forms a bow shock but is judged unrealistic. They conclude that the observed early ingress is not reproduced by the realistic scenario and that the bow-shock interpretation is disfavoured.

Significance. If the modelling assumptions are accepted, the paper contributes a quantitative, multi-fluid description of atmospheric escape and MgII absorption for WASP-12b, and it argues against the bow-shock explanation of the observed early ingress in favour of a stellar-capture regime. The model is more self-consistent than earlier prescribed-boundary 3D simulations in that it couples XUV-driven outflow, charge exchange, and minor-species ionization, and it produces specific predictions for absorption-line profiles and mass-loss rates that can be compared with future observations. However, the significance is substantially tempered by the axisymmetric geometry, which excludes the Coriolis force and aligns the stellar wind with the planet-star line, and by the fact that the closest match to the observed MgII absorption is obtained by varying the poorly constrained stellar wind density. These issues directly affect the central claim that the realistic scenario cannot produce early ingress.

major comments (3)
  1. [Section 2 and Appendix A] The axisymmetric 2D model omits the Coriolis force and assumes co-directionality of the stellar wind velocity and the XUV flux. For WASP-12b the Keplerian velocity V_K=226 km/s (stated in Section 3.2) is comparable to the adopted fast-wind speed V_SW=417 km/s in scenario 1, so the true interaction is oblique rather than axisymmetric. The two-stream structure and the resulting conclusion that scenario 1 produces no early ingress (Section 4) follow from this imposed symmetry. The manuscript's assertion that Coriolis spiraling is 'still small' at about 3 R_P (Section 4) is unquantified; using the stated expansion speeds of 5-10 km/s, the deflection angle Omega*r/v at r=3 R_P is of order 0.1-1 rad, and the associated transverse Doppler shifts are tens of km/s, comparable to the widths of the simulated MgII absorption profiles. The central claim that the realistic scenario cannot explain the early ingress is therefore not robust to this omitted leading physical effect.
  2. [Section 4, Figs. 6-7 and Table 1] The claimed reproduction of the observed ~4% MgII absorption is obtained by selecting stellar wind densities N_sw=3e4 and 3e5 cm^-3 from a small grid (Table 1) rather than from an independent constraint on WASP-12's wind. The abstract's statement that the simulations 'enable ... to reproduce the times of ingress and egress' is not supported by the presented light curves: in the realistic scenario 1 no early ingress is formed, while in scenario 2 the computed ingress coincides with the optical transit (Fig. 7b). The comparison with observations is therefore a fit, not a prediction, and it does not validate the model's geometry for the early-ingress phenomenon.
  3. [Section 2 and Appendix A] The MgII abundance and absorption are sensitive to several unconstrained inputs, including the low-energy Mg + He+ double charge-exchange cross-section, which the manuscript states is 'currently unknown', and the heating efficiency eta_h=0.5. These parameters directly control the MgII column density and hence the simulated absorption depth. The paper does not provide a sensitivity analysis over plausible ranges of these values, so the reported match to the observed 4% absorption cannot be distinguished from a parameterised fit rather than a robust model outcome.
minor comments (4)
  1. [References] The reference list contains a duplicated entry for Shaikhislamov et al. 2016 (two identical entries with the same journal and page numbers).
  2. [References] The bibliography entry 'Cubtz M., Saar S. H., Shkolnik E., 2010' appears to be a typo for 'Cuntz et al.'; the in-text citation 'Cuntz et al. 2000' does not have a matching reference-list entry.
  3. [Section 4, Eq. (1)-(2)] The notation in Eq. (1) is unclear: the integral limit 'StR' and the subscripts 'v,out' and 'v,transit' are not defined, and the intensity I is used without an explicit definition.
  4. [Conclusions] The concluding sentence states that absorption is dominated by 'resonant thermal line broadening', but the text in Section 4 and Eq. (11) indicate that the line wings are controlled by natural broadening; this wording should be checked for consistency.

Circularity Check

1 steps flagged · score 6.0 of 10

Predicted absence of early ingress/bow shock in the captured regime is imposed by the 2D axisymmetric geometry, not derived from the simulated physics.

  1. self definitional [Section 3.2 (quasi-axisymmetric limitation) and Section 4 (no-early-ingress conclusion); see also Appendix A]
    "One of the major limitations of the quasi-axisymmetric approximation for the tidally locked system is the assumption of co-directionality for the SW plasma and XUV flux. /// Our simulations do not lead to the formation of an early ingress in scenario 1, regardless of the adopted SW and XUV flux values, as the structure of the escaping material stream is rather symmetric. This is obviously connected to the nature of the 2D model."

    The model is 2D axisymmetric about the planet-star line: the cylindrical symmetry axis is the star-planet line, the SW flow is taken co-directional with the XUV flux, and the Coriolis force is not included. Early ingress requires absorbing material ahead of the planet in the direction of orbital motion, which is an azimuthal asymmetry about that axis. The paper's 'no early ingress' / 'no bow-shock' result in scenario 1 is therefore entailed by the imposed symmetry and co-directionality, not an independent outcome of the simulated escape physics. The authors acknowledge this immediately ('obviously connected to the nature of the 2D model'), but the statement is still used to argue that the bow-shock/early-ingress scenario is unrealistic.

full rationale

The central escape calculation is self-contained: the multi-fluid equations are given in Appendix A, and the double-stream / captured-by-the-star flow topology and the ~10^12 g/s mass-loss rates are computed from the stated XUV and SW inputs rather than fitted to the MgII observations. The MgII absorption comparison is a selected grid point ('closest match' to ~4%) rather than a parameter inversion, and the paper does not rename that match as a prediction; I therefore do not count it as fitted-input circularity. The main circular element is the use of the 2D axisymmetric geometry to conclude that the realistic captured regime produces no early ingress and no bow shock. Because the model excludes Coriolis force and aligns the SW with the planet-star line, the absence of leading-side, orbit-direction asymmetry is guaranteed by construction. The manuscript is unusually candid about this ('This is obviously connected to the nature of the 2D model' and 'A complete understanding ... requires self-consistent numerical simulations in a three-dimensional geometry'), which keeps the circularity partial rather than total. Score 6 reflects one load-bearing 'prediction' (no early ingress / no bow shock) that reduces by construction, while the central tidal-escape result retains independent computational content.

Assumptions & free parameters 6 free parameters · 8 assumptions · 0 invented entities

The central claims rest on the authors' previously developed multi-fluid model, assumed stellar wind parameters and XUV fluxes, and stated boundary conditions. The MgII absorption prediction depends on the assumed Mg abundance and on an empirically unknown low-energy cross-section, making the quantitative match to observations partially tuned. No new physical entities are introduced.

free parameters (6)
  • Stellar wind density N_sw = 3e4-3e5 cm^-3 (best match)
    The stellar wind density is not directly constrained for WASP-12b. The run that reproduces the observed ~4% MgII absorption uses N_sw=3e4 and 3e5 cm^-3, so the absorption match is a parameter fit (Section 4).
  • Heating efficiency eta_h = 0.5
    Assumed from qualitative analysis in Shaikhislamov et al. 2014; directly sets the XUV heating term in the energy equation (Appendix A).
  • Mg/H abundance at inner boundary = 3.7e-5
    Taken as solar abundance (Anders & Grevesse 1989); the resulting MgII column density and hence absorption scale with this choice.
  • Low-energy Mg + He+ double charge-exchange cross-section = unspecified/unknown
    The paper notes this cross-section at low energies is 'currently unknown' (Section 4), yet the MgI/MgII partition depends on it through the prescription of Shaikhislamov et al. 2018.
  • XUV flux at 1 AU = 5, 10, 20 erg cm^-2 s^-1
    Sampled from the observationally plausible range for WASP-12 (Salz et al. 2016); the mass loss and absorption vary with this input.
  • Stellar wind velocity and temperature = 417 km/s, 3.17 MK (scenario 1); 226 km/s, 1.4 MK (scenario 2)
    Chosen as representative fast/slow stellar wind conditions; scenario 2 uses the Keplerian orbital velocity as the wind velocity, breaking the co-directionality assumption.
assumptions (8)
  • standard math Hydrodynamic continuity, momentum, and energy equations (A.1-A.3) with ideal gas closure
    Background equations of fluid dynamics.
  • domain assumption Weakly magnetized / non-magnetized planet
    Section 1 states the model assumes a weakly magnetized planet; a strong planetary magnetic field would change the escape and absorption geometry.
  • domain assumption 2D axisymmetric geometry with circularly averaged centrifugal force and no Coriolis force
    Section 2 and Appendix A; this restricts validity to about 5 Rp and is acknowledged as a limitation for WASP-12b's fast orbital motion.
  • domain assumption Stellar wind flow and stellar XUV flux are co-directional
    Appendix A states this assumption; in reality the Keplerian orbital velocity (226 km/s) dominates the relative SW velocity, breaking the symmetry.
  • domain assumption Solar XUV spectrum (Tobiska 1993) is a proxy for WASP-12's spectrum
    Appendix A: 'for the solar type host star such as WASP-12b we use here as a proxy the spectrum of the Sun'.
  • domain assumption Inner boundary at observed optical radius with T=2500 K and p=1 mbar
    Section 2, initial condition; the choice is designed so that the XUV flux is fully absorbed.
  • domain assumption All charged species share the same temperature and velocity due to strong coupling
    Section 2 and Appendix A justify this by short Coulomb times and magnetic coupling; it allows a single proton fluid.
  • standard math Voigt profile absorption calculation as formulated in Eqs. (1)-(11)
    Standard line absorption physics, with an analytical approximation for the Voigt integral.

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Cite this review

Pith. "Pith review of Modelling atmospheric escape and MgII near-ultraviolet absorption of the highly irradiated hot Jupiter WASP-12b." pith.science (2026). https://pith.science/paper/MJXZBGML

@misc{pith2026190802527,
  author       = {Pith},
  title        = {Pith review of: Modelling atmospheric escape and MgII near-ultraviolet absorption of the highly irradiated hot Jupiter WASP-12b},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MJXZBGML}},
  note         = {Machine review of arXiv:1908.02527}
}
read the original abstract

We present two-dimensional multi-fluid numerical modelling of the upper atmosphere of the hot Jupiter WASP-12b. The model includes hydrogen chemistry, and self-consistently describes the expansion of the planetary upper atmosphere and mass loss due to intensive stellar irradiation, assuming a weakly magnetized planet. We simulate the planetary upper atmosphere and its interaction with the stellar wind (SW) with and without the inclusion of tidal force and consider different XUV irradiation conditions and SW parameters. With the inclusion of tidal force, even for a fast SW, the escaping planetary material forms two streams, propagating towards and away from the star. The atmospheric escape and related mass loss rate reaching the value of 10^12 gs^-1 appear to be mostly controlled by the stellar gravitational pull. We computed the column density and dynamics of MgII ions considering three different sets of SW parameters and XUV fluxes. The simulations enable to compute the absorption at the position of the Mg h line and to reproduce the times of ingress and egress. In case of a slow SW and without accounting for tidal force, the high orbital velocity leads to the formation of a shock approximately in the direction of the planetary orbital motion. In this case, mass loss is proportional to the stellar XUV flux. At the same time, ignoring of tidal effects for WASP-12b is a strong simplification, so the scenario with a shock, altogether is an unrealistic one.

Figures

Figures reproduced from arXiv: 1908.02527 by the authors.

Figure 1
Figure 1. Density distribution of planetary atoms nH (a, c, e) and planetary and SW protons nH+ (b, d, f) surrounding WASP-12b resulting from the simulations run within scenario 1. There are two panels for each considered stellar XUV flux: FXUV=5ergcm-2 s -1 (a, b), FXUV=10ergcm-2 s -1 (c, d), and FXUV=20ergcm-2 s -1 (e, f). The planet lies at the center of the coordinate system and the star is located in the direction of the… view at source ↗
Figure 5
Figure 5. Top row: same as [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Absorption line profile of the MgII h line in scenario 1 under three different stellar XUV flux levels: FXUV=5ergcm-2 s -1 (black), FXUV=10ergcm-2 s -1 (red), and FXUV=20ergcm-2 s -1 (blue), Panel (a): rarified SW ( 43 NSW 1 10 cm  and 43 NSW 1.5 10 cm  ); Panel (b): dense SW ( 43 NSW 3 10 cm  and 53 NSW 3 10 cm  ) [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figures from the paper (2 more)
Figure 7
Figure 7. Figure 7: Absorption line profile of the MgII h line (a) and transit light curves (b) derived from the simulations for the scenario 2 under over-dense SW ( 63 NSW 1 10 cm  ) and three different stellar XUV flux levels: FXUV=5ergcm-2 s -1 (black), FXUV=10ergcm-2 s -1 (red), an…
Figure 8
Figure 8. Figure 8: corresponds to the numerical model takeoff phase after a simulation start and before achieving the quasi-steady-state with the meaningful values. The average saturated values for the mass loss rate are listed in [PITH_FULL_IMAGE:figures/full_fig_p016_8.png]

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Works this paper leans on

34 extracted references · 33 canonical work pages

  1. [1]

    C., 2011, Astrophys

    Adams F. C., 2011, Astrophys. Journal, 730,

    work page 2011

  2. [3]

    García Muñoz A., 2007, P&SS, 55,

    work page 2007

  3. [9]

    E., Jackson A

    Owen, J. E., Jackson A. P., 2012, MNRAS, 425,

    work page 2012

  4. [19]

    V., Kaigorodov P., Konstantinova N

    Bisikalo D. V., Kaigorodov P., Konstantinova N. I., 2015, Astronomy Reports, 59, 829-835. Cubtz M., Saar S. H., Shkolnik E., 2010, Astrophys. Journal, 533, L151-L154. Bourrier, V., Lecavelier des Etangs A., 2013, A&A, 557, A124. Braginskii S. I., 1965, Rev. Plasma Phys., 1,

    work page 2015

  5. [25]

    G., & Stebbings R

    Lindsay B. G., & Stebbings R. F., 2005, JGRA, 110, A12213. Llama J., Wood K., Jardine M., Vidotto A. A., Helling Ch., Fossati L., Haswell C. A., 2011, Mont. Not. R. Astron. Sco. 416, L41-L44. Matsakos T., Uribe A., Konigl, A., 2015, Astronomy and Astrophysics, 578, A6. Meier E. T., Shumlak U., 2012, PhPl, 19, 072508. Murray-Clay R. A., Chiang E. I., Murra...

    work page 2005

  6. [27]

    Anders E., Grevesse N., 1989, GeCoA, 53,

    work page 1989

  7. [28]

    F., Khodachenko M

    Shaikhislamov I. F., Khodachenko M. L., Lammer H., Fossati L., Dwivedi N., Güdel M., Kislyakova K. G., Johnstone C. P., Berezutsky A. G., Miroshnichenko, Posukh V. G., Erkaev N. V., Ivanov V.A., 2018, Astrophys. Journal (Accepted). Shematovich V. I., 2012, Solar System Research, 46, 391-407. 20 Shkolnik E., Bohlender D. A., Walker G. A. H., Cameron A. C.,...

    work page 2018

  8. [50]

    L., Shaykhislamov I., Lammer H., Kislyakova K

    Khodachenko M. L., Shaykhislamov I., Lammer H., Kislyakova K. G., Fossati L., Johnstone C. P., Arkhypov O. V., Berezutsky A. G., Mi roshnichenko I. B., Posukh V. G., 2017, Astrophys. Journal, 847,

    work page 2017

Show all 34 references
  1. [52]

    C., Schmitt J

    Salz M., Czesla S., Schneider P. C., Schmitt J. H. M. M., 2016, Astronomy & Astrophysics, 586, A75. Shaikhislamov I. F., Khodachenko M. L., Sasunov Yu L., Lammer H., Kislyakova K. G., Erkaev N. V., 2014, Astrophys. Journal, 795,

    2016

  2. [70]

    L., Shaykhislamov I., Lammer H., Prokopov P

    Khodachenko M. L., Shaykhislamov I., Lammer H., Prokopov P. A., 2015, Astrophys. Journal, 813,

    2015

  3. [79]

    A., Bouchy F., Stempels H

    Hebb L., Collier-Cameron A., Loeillet B., Pollacco D., Hebrard G., Street R. A., Bouchy F., Stempels H. C., Moutou C., Simpson E., Udry S., Joshi Y. C., West R. G., Skillen I., Wilson D. M., McDonald I., Gibson N. P., Aigrain S., Anderson D. R., Benn C. R., Christian D. J., En...

    2009

  4. [98]

    H., 2013, Astrophys

    Guo J. H., 2013, Astrophys. Journal, 766,

    2013

  5. [102]

    A., Fossati L., Ayres T., France K., Froning C

    Haswell C. A., Fossati L., Ayres T., France K., Froning C. S., Holmes S., Kolb U. C., Busuttil R., Street R. A., Hebb L., Collier Cameron A., Enoch B., Burwitz V., Rodriguez J., West R. G., Pollacco D., Wheatley P. J., Carter, A., 2012, Astrophys. Journal, 760,

    2012

  6. [118]

    E., Haswell C

    Fossati L., Koskinen T., France K., Cubillos P. E., Haswell C. A., Holmes S., Lanza A. F., Pillitteri I., 2018, The Astronomical Journal 155,

    2018

  7. [126]

    K., Holmström, M, Lammer, H., et al., 2014, Science, 346,

    Kislyakova, G. K., Holmström, M, Lammer, H., et al., 2014, Science, 346,

    2014

  8. [132]

    F., Khodachenko M

    Shaikhislamov I. F., Khodachenko M. L., Lammer H., Fossati L., Johnstone C. P., Porkopov P. V., Berezutsky A. G., Zakharov Yu. P., Posukh V. G., 2016, Astrophys. Journal, 832,

    2016

  9. [143]

    M., Bourrier V., Désert J

    Vidal-Madjar A., Huitson C. M., Bourrier V., Désert J. M., Ballester G., des Etangs A. L., McConnell J. C., 2013, Astronomy & Astrophysics, 560, A54. Vidotto A. A., Jardine M., Helling Ch., 2010, Astrophys. Journal Letts., 722, L168-L172. Vidotto A. A., Llama J., Jardine M., H...

    2013

  10. [152]

    K., 1993, JGRA, 98, 18879

    Tobiska W. K., 1993, JGRA, 98, 18879. Verner D. A., Ferland G. J., Korista K. T., Yakovlev D. G., 1996, ApJ, 465,

    1993

  11. [157]

    C., Fortney Jonathan J., 2010, Nature, 463,

    Li Shu-lin, Miller N., Lin Douglas N. C., Fortney Jonathan J., 2010, Nature, 463,

    2010

  12. [167]

    L., Alexeev I

    Khodachenko M. L., Alexeev I. I., Belenkaya E., Lammer H., Grießmeier J.-M., Leitzinger M., Odert P., Zaqarashvili T., Rucker H. O., 2012, Astrophys. Journal, 744,

    2012

  13. [173]

    I., 2012, Solar System Research, 46, 391-407

    Shematovich V. I., 2012, Solar System Research, 46, 391-407. Shaikhislamov I. F., Khodachenko M. L., Lammer H., Fossati L., Johnstone C. P., Porkopov P. V., Berezutsky A. G., Zakharov Yu. P., Posukh V. G., 2016, Astrophys. Journal, 832,

    2012

  14. [197]

    Journal, 764,

    Bisikalo D., Kaygorodov P., Ionov D., Shematovich V., Lammer H., Fossati L., 2013, Astrophys. Journal, 764,

    2013

  15. [205]

    D., Physical Review A, 1986, 34(4),

    DuBois, R. D., Physical Review A, 1986, 34(4),

    1986

  16. [339]

    D., Wynn G

    Nichols J. D., Wynn G. A., Goad M., Alexander R. D., Casewell S. L., Cowley S. W. H, Burleigh M. R., Clarke J. T., Bisikalo D., 2015, Astrophys. Journal, 803,

    2015

  17. [487]

    M., Ballester G

    Vidal-Madjar A., Lecavelier des Etangs A., Désert J. M., Ballester G. E., Ferlet R., Hébrard G., Mayor M., 2003, Nature, 422,

    2003

  18. [515]

    Lai D., Helling Ch., van den Heuvel E. P. J. ,2010, Astrophys. Journal, 721, 923-928. Lammer H., Bredehöft J. H., Coustenis A., Khodachenko M. L., Kaltenegger L., Grasset O., Prieur D., Raulin F., Ehrenfreund P., Yamauchi M., Wahlund J. -E., Grießmeier J.-M., Stangl G., Cockel...

    2010

  19. [970]

    P., Güdel M., Lüftinger T., et al., 2015, Astronomy and Astrophys., 577, A27 Khodachenko M

    Johnstone C. P., Güdel M., Lüftinger T., et al., 2015, Astronomy and Astrophys., 577, A27 Khodachenko M. L., Lammer H., Lichtenegger H .I. M., Langmayr D., Erkaev N. V., Grießmeier J-M., Leitne M., Penz T., Biernat H. K., Motschmann U., Rucker H. O., 2007a, P&SS, 55,

    2015

  20. [981]

    T., Aylward A

    Koskinen T. T., Aylward A. D., Smith C. G. A., & Miller S., 2007., ApJ, 661(1),

    2007

  21. [1062]

    V., 2004, Icarus, 170, 167-179

    Yelle R. V., 2004, Icarus, 170, 167-179. Appendix A The Model Equations To simulate the dynamics of the escaping hydrogen dominated atmosphere of WASP-12b and its interaction with the SW, we employ a 2D axially symmetric hydrodynamic multi-fluid numerical model in the cylindri...

    2004

  22. [1426]

    H., 2011, Astrophys

    Guo J. H., 2011, Astrophys. Journal, 733,

    2011

  23. [1993]

    The spectrum is based on measurements of solar radiation under moderate activity conditions with proxy index

    and covering the range 10–912 Å, binned by 1 Å. The spectrum is based on measurements of solar radiation under moderate activity conditions with proxy index . It is assumed that the energy released in the form of photo-electrons is rapidly and equally re -distributed between a...

    2005

  24. [1996]

    2000, Nahar & Pradhan 1997)

    and recombination rates (Le Teuff et al. 2000, Nahar & Pradhan 1997). Note, that we do not consider chemical reactions among the different minor species, whereas the list of modeled hydrogen reactions is presented in Khodachenko et al. (2015), and it is practically the same as...

    2015

  25. [2738]

    Ehrenreich D., Bourrier V., Wheatley P

    Debrecht A., Carroll-Nellenback J., Frank A., Fossati L., Blackman Eric G., Dobbs -Dixon I., 2018, MNRAS, DOI 10.1093/mnras/sty1164. Ehrenreich D., Bourrier V., Wheatley P. J., Lecavelier des Etangs A., Hébrard G., Udry S., Bonfils X., Delfosse X., Désert J.-M., Sing D. K. , V...

    2018 doi

  26. [2931]

    J., Matsakos T., 2015, Astrophys

    Pillitteri I., Maggio A., Micela G., Sciortino S., Wolk S. J., Matsakos T., 2015, Astrophys. Journal, 805,

    2015

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