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Intro -- Was Sie in diesem essential finden können -- Vorwort -- Inhaltsverzeichnis -- 1 Einleitung -- 2 Speicher im Energiewirtschaftsrecht - Rechtsgrundlagen, Begriffe, Bedeutung -- 2.1 Rechtsgrundlagen -- 2.2 Grundlegendes zur Einordnung von Speichern -- 2.3 Begriffe -- 2.4 Speicher und Entflechtung (Unbundling) -- 2.5 Speicher in Zielen und Grundsätzen des EnWG -- 3 Stromnebenkosten bei der Speicherung -- 3.1 Netznutzungsentgelte -- 3.1.1 Freistellung für neue Anlagen zur Speicherung elektrischer Energie -- 3.1.2 Erweiterung für Power-to-Gas -- 3.1.3 Netzentgeltbefreiung für modernisierte Pumpspeicherwerke -- 3.1.4 Andere Befreiungstatbestände -- 3.2 EEG-Umlage -- 3.2.1 Befreiung für den Verbrauch in Stromspeichern im EEG 2017 -- 3.2.2 Befreiung für Power-to-Gas mit EE-Strom im EEG 2017 -- 3.2.3 Eigenversorgungsprivileg -- 3.3 Andere Umlagen und Abgaben, insbesondere KWK-Umlage -- 3.4 Stromsteuer -- 3.4.1 Anwendungserlass des BMF für Batteriespeicher -- 3.4.2 Befreiungstatbestände -- 3.5 Fazit und Ausblick -- 4 Rechtliche Rahmenbedingungen für die Marktteilnahme von Speichern -- 4.1 Netzanschluss von Speichern -- 4.1.1 Anschluss nach dem EnWG -- 4.1.2 Anschluss nach dem EEG -- 4.2 Vermarktungsmöglichkeiten im Energiewirtschaftsrecht -- 4.2.1 LieferverträgeBörsenhandel -- 4.2.2 Teilnahme an den Regelenergiemärkten -- 4.2.3 Speicher im Strommarkt 2.0 und im Strommarktgesetz -- 4.2.4 Entgelt für dezentrale Einspeisung -- 4.3 Vermarktungsmöglichkeiten im EEG 2017 -- 4.3.1 EEG-Förderung bei Rückverstromung und Einspeisung in ein Netz -- 4.3.2 EEG-Direktvermarktung und Speicher -- 4.3.3 Fördervoraussetzungen des EEG -- 4.3.4 Weitere Märkte -- 4.4 Förderprogramme -- 5 Recht für die Sektorkopplung -- 5.1 Grundlagen Sektorkopplung -- 5.2 Sektorkopplung im Klimaschutzplan und im EnWG -- 5.3 Entgelte, Abgaben und Umlagen bei der Sektorkopplung.

Höchste Zeit, dem Klimaschutz Vorschriften zu machen. Höchste Zeit für diesen neuen interdisziplinären Gesamtkommentar: Frenz, Klimaschutzrecht, der hochaktuell die ganze Komplexität eines der wichtigsten Gegenwartsthemen abbildet und deshalb neben den Erläuterungen der gesetzlichen Grundlagen auch in Querschnittsthemen einführt und unterschiedliche Sichtweisen berücksichtigt. Für Lösungen, die jetzt in der Praxis umsetzbar sind und in die Zukunft weisen!

Große Herausforderungen – starke Unterstützung: Wie dynamisch sich das Klimaschutzrecht derzeit entwickelt, zeigt die Neuauflage dieses Gesamtkommentars. Praxisnah und pointiert werden erneut die jüngsten Entwicklungen erläutert: Klimaschutz-Beschluss des BVerfG vom 24.03.2021, Nichtannahmebeschluss des BVerfG vom 18.01.2022, Novellierungen des KSG Bund und des KSG NRW, neues EU-Klimagesetz und EU-Klimapaket, Beginn der ersten Handelsperiode des BEHG, Ziele des Koalitionsvertrages der neuen Bundesregierung, Ergebnisse des Klimagipfels von Glasgow. Neben der Kommentierung des europäischen und nationalen Regelungsregimes werden auch die steuerrechtlichen Vorschriften und die verfassungsrechtlichen Hintergründe instruktiv beleuchtet. Weiterhin werden die interdisziplinären Querschnittsthemen gut verständlich dargestellt, darunter die ökonomischen, naturwissenschaftlichen und technischen Grundlagen. Dem Tempo der fortlaufenden Neuerungen wird auch ein digitales Add-on gerecht, über das Sie als Nutzerin und Nutzer des Werkes komfortabel weitere aktuelle Informationen abrufen können.

K2-18 is a nearby M2.5 dwarf, located at 34 pc and hosting a transiting planet that was first discovered by the K2 mission and later confirmed with Spitzer Space Telescope observations. With a radius of ∼2 R and an orbital period of ∼33 days, the planet lies in the temperate zone of its host star and receives stellar irradiation similar to that of Earth. Here we perform radial velocity follow-up observations with the visual channel of CARMENES with the goal of determining the mass and density of the planet. We measure a planetary semi-amplitude of K ∼ 3.5 and a mass of M ∼ 9 M , yielding a bulk density around . This indicates a low-mass planet with a composition consistent with a solid core and a volatile-rich envelope. A signal at 9 days was recently reported using radial velocity measurements taken with the HARPS spectrograph. This was interpreted as being due to a second planet. We see a weaker, time- and wavelength-dependent signal in the CARMENES data set and thus favor stellar activity for its origin. K2-18 b joins the growing group of low-mass planets detected in the temperate zone of M dwarfs. The brightness of the host star in the near-infrared makes the system a good target for detailed atmospheric studies with the James Webb Space Telescope.K2-18 is a nearby M2.5 dwarf, located at 34 pc and hosting a transiting planet that was first discovered by the K2 mission and later confirmed with Spitzer Space Telescope observations. With a radius of similar to 2 R-circle plus and an orbital period of similar to 33 days, the planet lies in the temperate zone of its host star and receives stellar irradiation similar to that of Earth. Here we perform radial velocity follow-up observations with the visual channel of CARMENES with the goal of determining the mass and density of the planet. We measure a planetary semi-amplitude of K-b similar to 3.5 m s(-1). and a mass of M-b similar to 9 M-circle plus, yielding a bulk density around rho(b) similar to 4 g cm(-3). This indicates a low-mass planet with a composition consistent with a solid core and a volatile-rich envelope. A signal at 9 days was recently reported using radial velocity measurements taken with the HARPS spectrograph. This was interpreted as being due to a second planet. We see a weaker, time-and wavelength-dependent signal in the CARMENES data set and thus favor stellar activity for its origin. K2-18 b joins the growing group of low-mass planets detected in the temperate zone of M dwarfs. The brightness of the host star in the near-infrared makes the system a good target for detailed atmospheric studies with the James Webb Space Telescope.© 2018. The American Astronomical Society. ; CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia, and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation (DFG), the states of Baden-Wurttemberg and Niedersachsen, and the Junta de Andalucia. P.S. would like to thank Christoph Mordasini for his helpful comments on an early draft and Sudeshna Boro-Saikia for her help on calculating the calcium indices of the HARPS data set. I.R. and J.C.M. acknowledge support by the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grant ESP2016-80435-C2-1-R, as well as the support of the Generalitat de Catalunya/CERCA program. A.P.H. acknowledges the support of the Deutsche Forschungsgemeinschaft (DFG) grant HA 3279/11-1. J.A.C., P.J.A. and D.M. acknowledge support by the Spanish Ministry of Economy and Competitiveness (MINECO) from projects AYA2016-79425-C3-1, 2, 3-P. V.J.S.B. is supported by program AYA2015-69350-C3-2-P from Spanish Ministry of Economy and Competitiveness (MINECO). We thank the anonymous referee for useful comments that improved the paper.

Wir lichten den Nebel. Der brandneue Kommentar zum BImSchG erfasst eines der praxisrelevantesten Gebiete des Umweltrechts in seiner ganzen Dimension: sämtliche Vorschriften des BImSchG und die wichtigsten Vorschriften aus dem ausufernden untergesetzlichen Regelwerk. Die Änderungen durch das Gesetz zur Beschleunigung von Investitionen sowie beim Planungssicherstellungsgesetz sind bereits berücksichtigt. Enthalten ist auch eine Vorschau auf die laufende Umsetzung der Erneuerbaren-Energien-Richtlinie. Alles komfortabel versammelt in einem handlichen Werk mit präzisen, klar verständlichen Erläuterungen auf dem neuesten Stand der Rechtsprechung – verschaffen Sie sich jetzt den Überblick!

Statistical analysis of velocity fluctuations in the interstellar medium (ISM) of the Milky Way and NGC 4321 show that the motion of molecular gas over scales ranging from 0.1 to 1,000 pc is similar, and consistent with that generated by a combination of gravity and turbulence. ISM structure at one scale is therefore linked to structure at other scales. The density structure of the interstellar medium determines where stars form and release energy, momentum and heavy elements, driving galaxy evolution(1-4). Density variations are seeded and amplified by gas motion, but the exact nature of this motion is unknown across spatial scales and galactic environments(5). Although dense star-forming gas probably emerges from a combination of instabilities(6,7), convergent flows(8)and turbulence(9), establishing the precise origin is challenging because it requires gas motion to be quantified over many orders of magnitude in spatial scale. Here we measure(10-12)the motion of molecular gas in the Milky Way and in nearby galaxy NGC 4321, assembling observations that span a spatial dynamic range 10(-1)-10(3) pc. We detect ubiquitous velocity fluctuations across all spatial scales and galactic environments. Statistical analysis of these fluctuations indicates how star-forming gas is assembled. We discover oscillatory gas flows with wavelengths ranging from 0.3-400 pc. These flows are coupled to regularly spaced density enhancements that probably form via gravitational instabilities(13,14). We also identify stochastic and scale-free velocity and density fluctuations, consistent with the structure generated in turbulent flows(9). Our results demonstrate that the structure of the interstellar medium cannot be considered in isolation. Instead, its formation and evolution are controlled by nested, interdependent flows of matter covering many orders of magnitude in spatial scale. ; German Research Foundation (DFG) KR4801/1-1 KR4801/2-1 European Research Council (ERC) 714907 European Union's Horizon 2020 research and innovation program 639459 National Science Foundation (NSF) 1615105 1615109 1653300 NASA under ADAP NNX16AF48G NNX17AF39G Natural Sciences and Engineering Research Council of Canada RGPIN-2017-03987 National Science Foundation (NSF) 1816715 AST-9800334 AST-0098562 AST-0100793 AST-0228993 AST-0507657 German Research Foundation (DFG) SFB 881 Heidelberg Cluster of Excellence STRUCTURES of Germany's Excellence Strategy EXC-2181/1-390900948 ERC under the European Union's Horizon 2020 research and innovation programme 694343 European Union's Horizon 2020 research and innovation programme 726384 Programme National 'Physique et Chimie du Milieu Interstellaire' (PCMI) of CNRS/INSU INC/INP French Atomic Energy Commission Centre National D'etudes Spatiales Australian Government Australian Research Council UNSW, Sydney Monash Universities Commonwealth Scientific & Industrial Research Organisation (CSIRO)

Hot gas giant exoplanets can lose part of their atmosphere due to strong stellar irradiation, and these losses can affect their physical and chemical evolution. Studies of atmospheric escape from exoplanets have mostly relied on space-based observations of the hydrogen Lyman-a line in the far ultraviolet region, which is strongly affected by interstellar absorption. Using ground-based high-resolution spectroscopy, we detected excess absorption in the helium triplet at 1083 nanometers during the transit of the Saturn-mass exoplanet WASP-69b, at a signal-to-noise ratio of 18. We measured line blueshifts of several kilometers per second and posttransit absorption, which we interpret as the escape of part of the atmosphere trailing behind the planet in comet-like form.© 2018 American Association for the Advancement of Science. All rights reserved. ; CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia, and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and Deutsche Forschungsgesellschaft (DFG) Research Unit FOR2544 >Blue Planets around Red Stars,> the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. We acknowledge funding from the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grants ESP2016-80435-C2-1-R, ESP 2016-76076-R, ESP2014-54362-P, ESP 2014-54062-R, AYA2016-79425-C3-2-P, AYA2016-79425-C3-1-P, AYA2016-79425C3-2-P, AYA2014-54348-C3-1-R, and AYA2016-79425-C3-3-P. We also acknowledge funding through the DFG through grants DFG DR281/32-1, RE 1664/14-1, DFG SFB 676, and DFG SCHM 1032/57-1 and by the Deutsches Zentrum fur Luft und Raumfahrt (DLR) through grants DLR 50 OR 1710, DLR 50 OR 1307, and BMWi50OR1505, as well as the support of the Generalitat de Catalunya/CERCA program. I.A.G.S. and F.J.A.-F. acknowledge funding from the research program VICI 639.043.107 funded by the Dutch Organisation for Scientific Research (NWO) and funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program under grant agreement 694513. G.C. acknowledges support by the National Natural Science Foundation of China (grant 11503088) and the Natural Science Foundation of Jiangsu Province (grant BK20151051).

We report the period, eccentricity, and mass determination for the Transiting Exoplanet Survey Satellite (TESS) single-transit event candidate TOI-222, which displayed a single 3000 ppm transit in the TESS 2-min cadence data from Sector 2. We determine the orbital period via radial velocity measurements (P = 33.9 d), which allowed for ground-based photometric detection of two subsequent transits. Our data show that the companion to TOI-222 is a low-mass star, with a radius of 0.18(-0.10)(+0.39) R-circle dot and a mass of 0.23 +/- 0.01 M-circle dot. This discovery showcases the ability to efficiently discover long-period systems from TESS single-transit events using a combination of radial velocity monitoring coupled with high-precision ground-based photometry. ; Swiss National Science Foundation (SNSF) Geneva University Swiss National Science Foundation (SNSF) Science & Technology Facilities Council (STFC) ST/M001962/1 ST/S002642/1 Science & Technology Facilities Council (STFC) ST/L000733/1 ST/P000495/1 ST/N000757/1 ST/P000312/1 1226157 STFC via an Ernest Rutherford Fellowship ST/R00384X/1 MIT's Kavli Institute Austrian Research Promotion Agency (FFG) 859724 Comisión Nacional de Investigación Científica y Tecnológica (CONICYT) PB06 CONICYT-PFCHA, Chile 21191829 Millennium Institute of Astrophysics (MAS) Comisión Nacional de Investigación Científica y Tecnológica (CONICYT) CONICYT FONDECYT 1161218 3180246 1171208 Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio IC120009 European Research Council (ERC) 681601 ERC under the European Union 320964 Australian Research Council LE160100001 DP180100972 Mount Cuba Astronomical Foundation University of Texas at Austin UNSW Australia MIT Nanjing University George Mason University University of Louisville University of California System University of Florida NASA's Science Mission directorate University of Southern Queensland