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  • 1
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    A new model suite to determine the influence of cosmic rays on (exo)planetary atmospheric biosignatures : Validation based on modern Earth
    EDP Sciences ; 2019
    In:  Astronomy & Astrophysics Vol. 631 ( 2019-11), p. A101-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 631 ( 2019-11), p. A101-
    Abstract: Context. The first opportunity to detect indications for life outside of the Solar System may be provided already within the next decade with upcoming missions such as the James Webb Space Telescope (JWST), the European Extremely Large Telescope (E-ELT) and the Atmospheric Remote-sensing Infrared Exoplanet Large-survey (ARIEL) mission, searching for atmospheric biosignatures on planets in the habitable zone of cool K- and M-stars. Nevertheless, their harsh stellar radiation and particle environment could lead to photochemical loss of atmospheric biosignatures. Aims. We aim to study the influence of cosmic rays on exoplanetary atmospheric biosignatures and the radiation environment considering feedbacks between energetic particle precipitation, climate, atmospheric ionization, neutral and ion chemistry, and secondary particle generation. Methods. We describe newly combined state-of-the-art modeling tools to study the impact of the radiation and particle environment, in particular of cosmic rays, on atmospheric particle interaction, atmospheric chemistry, and the climate-chemistry coupling in a self-consistent model suite. To this end, models like the Atmospheric Radiation Interaction Simulator (AtRIS), the Exoplanetary Terrestrial Ion Chemistry model (ExoTIC), and the updated coupled climate-chemistry model are combined. Results. In addition to comparing our results to Earth-bound measurements, we investigate the ozone production and -loss cycles as well as the atmospheric radiation dose profiles during quiescent solar periods and during the strong solar energetic particle event of February 23, 1956. Further, the scenario-dependent terrestrial transit spectra, as seen by the NIR-Spec infrared spectrometer onboard the JWST, are modeled. Amongst others, we find that the comparatively weak solar event drastically increases the spectral signal of HNO 3 , while significantly suppressing the spectral feature of ozone. Because of the slow recovery after such events, the latter indicates that ozone might not be a good biomarker for planets orbiting stars with high flaring rates.
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/201935888
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2019
    detail.hit.zdb_id: 1458466-9
    SSG: 16,12
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  • 2
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    From solar to stellar flare characteristics : On a new peak size distribution for G-, K-, and M-dwarf star flares
    EDP Sciences ; 2019
    In:  Astronomy & Astrophysics Vol. 621 ( 2019-01), p. A67-
    Details
    In: Astronomy & Astrophysics, EDP Sciences, Vol. 621 ( 2019-01), p. A67-
    Abstract: Context. The connection between solar energetic proton events and X-ray flares has been the focus of many studies over the past 13 yr. In the course of these investigations several peak size distribution functions based on Geostationary Operational Environmental Satellite (GOES) measurements of both quantities have been developed. In more recent studies one of these functions has been used to estimate the stellar proton fluence around the M-dwarf star AD Leonis. However, a comparison of the existing peak size distribution functions reveals strong discrepancies with respect to each other. Aims. The aim of this paper is to derive a new peak size distribution function that can be utilized to give a more realistic estimate of the stellar proton flux of G-, K-, and M-dwarf stars. Methods. By updating and extending the GOES-based peak size distribution down to B-class X-ray flare intensities with the help of SphinX data from the solar minimum conditions of 2009 and newly derived GOES data between 1975 and 2005, we developed a new power-law peak size distribution function for solar proton fluxes ( E   〉  10 MeV). However, its resulting slope differs from values reported in the literature. Therefore, we also developed a double-power-law peak size distribution function. An extension to much higher X-ray flare intensities (10 −1 ) W m −2 and above, for the first time, results in an approximation of best- and worst-case scenarios of the stellar proton flux around G-, K-, and M-dwarf stars. Results. Investigating the impact of the newly developed peak size distribution function for G-, K-, and M-dwarf star flare intensities we show that in the worst-case scenario previous studies may underestimate the stellar proton flux by roughly one to five orders of magnitude.
    Type of Medium: Online Resource
    ISSN: 0004-6361 , 1432-0746
    URL: Article
    DOI: 10.1051/0004-6361/201832789
    RVK:
    UA 1000
    RVK:
    US 1090
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2019
    detail.hit.zdb_id: 1458466-9
    SSG: 16,12
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  • 3
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    Study of the Ground Level Enhancements effect on atmospheric electric properties and mineral dust particle charging
    Elsevier BV ; 2022
    In:  Journal of Atmospheric and Solar-Terrestrial Physics Vol. 233-234 ( 2022-07), p. 105871-
    Details
    In: Journal of Atmospheric and Solar-Terrestrial Physics, Elsevier BV, Vol. 233-234 ( 2022-07), p. 105871-
    Type of Medium: Online Resource
    ISSN: 1364-6826
    URL: Article
    DOI: 10.1016/j.jastp.2022.105871
    RVK:
    UA 4547.8
    Language: English
    Publisher: Elsevier BV
    Publication Date: 2022
    detail.hit.zdb_id: 2020910-1
    SSG: 16,13
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  • 4
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    EUropean Heliospheric FORecasting Information Asset 2.0
    EDP Sciences ; 2020
    In:  Journal of Space Weather and Space Climate Vol. 10 ( 2020), p. 57-
    Details
    In: Journal of Space Weather and Space Climate, EDP Sciences, Vol. 10 ( 2020), p. 57-
    Abstract: Aims : This paper presents a H2020 project aimed at developing an advanced space weather forecasting tool, combining the MagnetoHydroDynamic (MHD) solar wind and coronal mass ejection (CME) evolution modelling with solar energetic particle (SEP) transport and acceleration model(s). The EUHFORIA 2.0 project will address the geoeffectiveness of impacts and mitigation to avoid (part of the) damage, including that of extreme events, related to solar eruptions, solar wind streams, and SEPs, with particular emphasis on its application to forecast geomagnetically induced currents (GICs) and radiation on geospace. Methods : We will apply innovative methods and state-of-the-art numerical techniques to extend the recent heliospheric solar wind and CME propagation model EUHFORIA with two integrated key facilities that are crucial for improving its predictive power and reliability, namely (1) data-driven flux-rope CME models, and (2) physics-based, self-consistent SEP models for the acceleration and transport of particles along and across the magnetic field lines. This involves the novel coupling of advanced space weather models. In addition, after validating the upgraded EUHFORIA/SEP model, it will be coupled to existing models for GICs and atmospheric radiation transport models. This will result in a reliable prediction tool for radiation hazards from SEP events, affecting astronauts, passengers and crew in high-flying aircraft, and the impact of space weather events on power grid infrastructure, telecommunication, and navigation satellites. Finally, this innovative tool will be integrated into both the Virtual Space Weather Modeling Centre (VSWMC, ESA) and the space weather forecasting procedures at the ESA SSCC in Ukkel (Belgium), so that it will be available to the space weather community and effectively used for improved predictions and forecasts of the evolution of CME magnetic structures and their impact on Earth. Results : The results of the first six months of the EU H2020 project are presented here. These concern alternative coronal models, the application of adaptive mesh refinement techniques in the heliospheric part of EUHFORIA, alternative flux-rope CME models, evaluation of data-assimilation based on Karman filtering for the solar wind modelling, and a feasibility study of the integration of SEP models.
    Type of Medium: Online Resource
    ISSN: 2115-7251
    URL: Article
    DOI: 10.1051/swsc/2020055
    Language: English
    Publisher: EDP Sciences
    Publication Date: 2020
    detail.hit.zdb_id: 2628166-1
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  • 5
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    Osimertinib in Resected EGFR -Mutated Non–Small-Cell Lung Cancer
    Massachusetts Medical Society ; 2020
    In:  New England Journal of Medicine Vol. 383, No. 18 ( 2020-10-29), p. 1711-1723
    Details
    In: New England Journal of Medicine, Massachusetts Medical Society, Vol. 383, No. 18 ( 2020-10-29), p. 1711-1723
    Type of Medium: Online Resource
    ISSN: 0028-4793 , 1533-4406
    URL: Article
    DOI: 10.1056/NEJMoa2027071
    RVK:
    XA 10000
    Language: English
    Publisher: Massachusetts Medical Society
    Publication Date: 2020
    detail.hit.zdb_id: 1468837-2
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  • 6
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    Adjuvant Osimertinib for Resected EGFR-Mutated Stage IB-IIIA Non–Small-Cell Lung Cancer: Updated Results From the Phase III Randomized ADAURA Trial
    American Society of Clinical Oncology (ASCO) ; 2023
    In:  Journal of Clinical Oncology Vol. 41, No. 10 ( 2023-04-01), p. 1830-1840
    Details
    In: Journal of Clinical Oncology, American Society of Clinical Oncology (ASCO), Vol. 41, No. 10 ( 2023-04-01), p. 1830-1840
    Abstract: Clinical trials frequently include multiple end points that mature at different times. The initial report, typically based on the primary end point, may be published when key planned co-primary or secondary analyses are not yet available. Clinical Trial Updates provide an opportunity to disseminate additional results from studies, published in JCO or elsewhere, for which the primary end point has already been reported. PURPOSE The phase III ADAURA (ClinicalTrials.gov identifier: NCT02511106 ) primary analysis demonstrated a clinically significant disease-free survival (DFS) benefit with adjuvant osimertinib versus placebo in EGFR-mutated stage IB-IIIA non–small-cell lung cancer (NSCLC) after complete tumor resection (DFS hazard ratio [HR], 0.20 [99.12% CI, 0.14 to 0.30] ; P 〈 .001). We report an updated exploratory analysis of final DFS data. METHODS Overall, 682 patients with stage IB-IIIA (American Joint Committee on Cancer/Union for International Cancer Control, seventh edition) EGFR-mutated (exon 19 deletion/L858R) NSCLC were randomly assigned 1:1 (stratified by stage, mutational status, and race) to receive osimertinib 80 mg once-daily or placebo for 3 years. The primary end point was DFS by investigator assessment in stage II-IIIA disease analyzed by stratified log-rank test; following early reporting of statistical significance in DFS, no further formal statistical testing was planned. Secondary end points included DFS in stage IB-IIIA, overall survival, and safety. Patterns of recurrence and CNS DFS were prespecified exploratory end points. RESULTS At data cutoff (April 11, 2022), in stage II-IIIA disease, median follow-up was 44.2 months (osimertinib) and 19.6 months (placebo); the DFS HR was 0.23 (95% CI, 0.18 to 0.30); 4-year DFS rate was 70% (osimertinib) and 29% (placebo). In the overall population, DFS HR was 0.27 (95% CI, 0.21 to 0.34); 4-year DFS rate was 73% (osimertinib) and 38% (placebo). Fewer patients treated with osimertinib had local/regional and distant recurrence versus placebo. CNS DFS HR in stage II-IIIA was 0.24 (95% CI, 0.14 to 0.42). The long-term safety profile of osimertinib was consistent with the primary analysis. CONCLUSION These updated data demonstrate prolonged DFS benefit over placebo, reduced risk of local and distant recurrence, improved CNS DFS, and a consistent safety profile, supporting the efficacy of adjuvant osimertinib in resected EGFR-mutated NSCLC.
    Type of Medium: Online Resource
    ISSN: 0732-183X , 1527-7755
    URL: Article
    DOI: 10.1200/JCO.22.02186
    RVK:
    XA 52760
    RVK:
    XA 10000
    Language: English
    Publisher: American Society of Clinical Oncology (ASCO)
    Publication Date: 2023
    detail.hit.zdb_id: 2005181-5
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  • 7
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    Astrospheres of Planet-Hosting Cool Stars and Beyond ⋅ When Modeling Meets Observations
    Springer Science and Business Media LLC ; 2022
    In:  Space Science Reviews Vol. 218, No. 4 ( 2022-06)
    Details
    In: Space Science Reviews, Springer Science and Business Media LLC, Vol. 218, No. 4 ( 2022-06)
    Abstract: Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and the structure of the heliosphere. Additionally, with the help of multi-wavelength observations by the Hubble Space Telescope , Kepler , and TESS , we not only were able to detect a variety of extrasolar planets and exomoons but also to study the characteristics of their host stars, and thus became aware that other stars drive bow shocks and astrospheres. Although features like, e.g., stellar winds, could not be measured directly, over the past years several techniques have been developed allowing us to indirectly derive properties like stellar mass-loss rates and stellar wind speeds, information that can be used as direct input to existing astrospheric modeling codes. In this review, the astrospheric modeling efforts of various stars will be presented. Starting with the heliosphere as a benchmark of astrospheric studies, investigating the paleo-heliospheric changes and the Balmer $\text{H}\upalpha$ H α projections to $1~\text{pc}$ 1 pc , we investigate the surroundings of cool and hot stars, but also of more exotic objects like neutron stars. While pulsar wind nebulae (PWNs) might be a source of high-energy galactic cosmic rays (GCRs), the astrospheric environments of cool and hot stars form a natural shield against GCRs. Their modulation within these astrospheres, and the possible impact of turbulence, are also addressed. This review shows that all of the presented modeling efforts are in excellent agreement with currently available observations.
    Type of Medium: Online Resource
    ISSN: 0038-6308 , 1572-9672
    URL: Article
    DOI: 10.1007/s11214-022-00894-3
    Language: English
    Publisher: Springer Science and Business Media LLC
    Publication Date: 2022
    detail.hit.zdb_id: 2017804-9
    detail.hit.zdb_id: 2561549-X
    SSG: 16,12
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  • 8
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    Unusual Plasma and Particle Signatures at Mars and STEREO-A Related to CME–CME Interaction
    American Astronomical Society ; 2019
    In:  The Astrophysical Journal Vol. 880, No. 1 ( 2019-07-19), p. 18-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 880, No. 1 ( 2019-07-19), p. 18-
    Type of Medium: Online Resource
    ISSN: 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ab27ca
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2019
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
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  • 9
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    Health-Related Quality of Life Outcomes in Patients with Resected Epidermal Growth Factor Receptor–Mutated Non–Small Cell Lung Cancer Who Received Adjuvant Osimertinib in the Phase III ADAURA Trial
    American Association for Cancer Research (AACR) ; 2022
    In:  Clinical Cancer Research Vol. 28, No. 11 ( 2022-06-01), p. 2286-2296
    Details
    In: Clinical Cancer Research, American Association for Cancer Research (AACR), Vol. 28, No. 11 ( 2022-06-01), p. 2286-2296
    Abstract: In the phase III ADAURA trial, adjuvant treatment with osimertinib versus placebo, with/without prior adjuvant chemotherapy, resulted in a statistically significant and clinically meaningful disease-free survival benefit in completely resected stage IB–IIIA EGFR-mutated (EGFRm) non–small cell lung cancer (NSCLC). We report health-related quality of life (HRQoL) outcomes from ADAURA. Patients and Methods: Patients randomized 1:1 received oral osimertinib 80 mg or placebo for 3 years or until recurrence/discontinuation. HRQoL (secondary endpoint) was measured using the Short Form-36 (SF-36) health survey at baseline, 12, and 24 weeks, then every 24 weeks until recurrence or treatment completion/discontinuation. Exploratory analyses of SF-36 score changes from baseline until week 96 and time to deterioration (TTD) were performed in the overall population (stage IB–IIIA; N = 682). Clinically meaningful changes were defined using the SF-36 manual. Results: Baseline physical/mental component summary (PCS/MCS) scores were comparable between osimertinib and placebo (range, 46–47) and maintained to Week 96, with no clinically meaningful differences between arms; difference in adjusted least squares (LS) mean [95% confidence intervals (CI), −1.18 (−2.02 to −0.34) and −1.34 (−2.40 to −0.28), for PCS and MCS, respectively. There were no differences between arms for TTD of PCS and MCS; HR, 1.17 (95% CI, 0.82–1.67) and HR, 0.98 (95% CI, 0.70–1.39), respectively. Conclusions: HRQoL was maintained with adjuvant osimertinib in patients with stage IB–IIIA EGFRm NSCLC, who were disease-free after complete resection, with no clinically meaningful differences versus placebo, further supporting adjuvant osimertinib as a new treatment in this setting. See related commentary by Patil and Bunn, p. 2204
    Type of Medium: Online Resource
    ISSN: 1078-0432 , 1557-3265
    URL: Article
    DOI: 10.1158/1078-0432.CCR-21-3530
    RVK:
    XA 36791
    Language: English
    Publisher: American Association for Cancer Research (AACR)
    Publication Date: 2022
    detail.hit.zdb_id: 1225457-5
    detail.hit.zdb_id: 2036787-9
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  • 10
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    Revisiting the Revisited Palmer Consensus: New Insights from Jovian Electron Transport
    American Astronomical Society ; 2022
    In:  The Astrophysical Journal Vol. 929, No. 1 ( 2022-04-01), p. 8-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 929, No. 1 ( 2022-04-01), p. 8-
    Abstract: Novel insights into the behavior of the diffusion coefficients of charged particles in the inner heliosphere are of great importance to any study of the transport of these particles and are especially relevant with regard to the transport of low-energy electrons. The present study undertakes an exhaustive investigation into the diffusion parameters needed to reproduce low-energy electron intensities as observed at Earth, using a state-of-the-art 3D cosmic ray transport code. To this end, the transport of Jovian electrons is considered, as Jupiter represents the predominant source of these particles in the inner heliosphere, and because a careful comparison of model results with observations taken during periods of good and poor magnetic connectivity between Earth and Jupiter allows for conclusions to be drawn as to both parallel and perpendicular diffusion coefficients. This study then compares these results with the predictions made by various scattering theories. Best-fit parameters for parallel and perpendicular mean free paths at 1 au fall reasonably well within the span of observational values reported by previous studies, but best-fit radial and rigidity dependences vary widely. However, a large number of diffusion parameters lead to reasonable to-good fits to observations, and it is argued that considerable caution must be exercised when comparing theoretical results for diffusion coefficients with diffusion parameters calculated from particle transport studies.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ac58f5
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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