The Relevance of Digital Sharing Business Models for Sustainability

There is a growing discussion about the "Digital Sharing Economy" (DSE). The pervasiveness of digital platforms and the growing interest in a sharing (rather than ownership) style of consumption have allowed for sharing practices to scale up and become a widespread phenomenon. Digital sharing platforms offer a wide variety of services which appear to be more affordable, efficient, and accessible than their conventional counterparts, making them more attractive in the eyes of consumers. The DSE has manifested itself most remarkably in consumer-to-consumer (C2C) and business-to-consumer (B2C) sharing models. New business models have been created to capture and offer the values driving the emerging sharing trend. The innovative, digitally enabled mode of providing access to resources as a service in the DSE has changed consumption patterns both at micro level, as a change in individual lifestyles, and at macro level, manifested in a transformation of socio-economic structures. These ongoing changes may have both positive and negative implications for society from a sustainability perspective. Recognising that the (potential and actual) impacts of sharing platforms on sustainability have not been studied in a systematic way yet, the present paper aims to develop a systematic insight into this interaction by focusing on the business models emerging around sharing platforms as a central starting point. To achieve this, we use a typology of business models that recognizes the affordances and key attributes of sharing in the DSE. The typology covers both C2C and B2C models of sharing. Based on this typology, we discuss the implications of each type of sharing model for sustainability by asking two central questions: How may the given type of sharing affect resource consumption? And what will be the potential impacts on social practices and structures? We hope that the present study can serve as a guideline for assessing the sustainability impacts of sharing platforms -- either already operating in the market or envisaged. By highlighting the aspects most relevant from a sustainability point of view, we expect to contribute to an evolution of the DSE business models towards sustainable development

2nd ESMO Consensus Conference on Lung Cancer: early-stage non-small-cell lung cancer consensus on diagnosis, treatment and follow-up

This manuscript provides recommendations for the diagnosis, treatment and follow-up of early stage non-small cell lung cancer developed during the 2nd ESMO Consensus Conference on Lung Cancer in May 201

GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses

We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO’s and Virgo’s third observing run. The signal was recorded on April 12, 2019 at 05∶30∶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ∼30 M_⊙ black hole merged with a ∼8 M_⊙ black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein’s general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs

Properties and Astrophysical Implications of the 150 M_⊙ Binary Black Hole Merger GW190521

The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85⁺²¹₋₁₄ M_⊙ and 66⁺¹⁷₋₁₈ M_⊙, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65–120 M_⊙. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger 142⁺²⁸₋₁₆ M_⊙) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be 0.13_(-0.11)^(+0.30) Gpc⁻³ yr⁻¹. We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary

GW190521 : a binary black hole merger with a total mass of 150 M⊙

On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85+21−14  M⊙ and 66+17−18  M⊙ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65  M⊙. We calculate the mass of the remnant to be 142+28−16  M⊙, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3+2.4−2.6  Gpc, corresponding to a redshift of 0.82+0.28−0.34. The inferred rate of mergers similar to GW190521 is 0.13+0.30−0.11  Gpc−3 yr−1