YSOVAR: Mid-infrared Variability in NGC 1333

As part of the Young Stellar Object VARiability (YSOVAR) program, wemonitored NGC 1333 for ∼35 days at 3.6 and 4.5 μm using theSpitzer Space Telescope. We report here on the mid-infrared variabilityof the point sources in the ∼10‧ × ∼20‧ areacentered on 03:29:06, +31:19:30 (J2000). Out of 701 light curves ineither channel, we find 78 variables over the YSOVAR campaign. Abouthalf of the members are variable. The variable fraction for the mostembedded spectral energy distributions (SEDs) (Class I, flat) is higherthan that for less embedded SEDs (Class II), which is in turn higherthan the star-like SEDs (Class III). A few objects have amplitudes(10–90th percentile brightness) in [3.6] or [4.5] > 0.2 mag; amore typical amplitude is 0.1–0.15 mag. The largest color changeis >0.2 mag. There are 24 periodic objects, with 40% of them beingflat SED class. This may mean that the periodic signal is primarily fromthe disk, not the photosphere, in those cases. We find 9 variableslikely to be “dippers,” where texture in the disk occultsthe central star, and 11 likely to be “bursters,” whereaccretion instabilities create brightness bursts. There are 39 objectsthat have significant trends in [3.6]–[4.5] color over thecampaign, about evenly divided between redder-when-fainter (consistentwith extinction variations) and bluer-when-fainter. About a third of the17 Class 0 and/or jet-driving sources from the literature are variableover the YSOVAR campaign, and a larger fraction (∼half) are variablebetween the YSOVAR campaign and the cryogenic-era Spitzer observations(6–7 years), perhaps because it takes time for the envelope torespond to changes in the central source. The NGC 1333 brown dwarfs donot stand out from the stellar light curves in any way except there is amuch larger fraction of periodic objects (∼60% of variable browndwarfs are periodic, compared to ∼30% of the variables overall).

Where are the mid-sized flares of ultracool M dwarfs?

We propose to observe the M8.5 dwarf SCR J1845-6357 with XMM-Newton EPIC for 60 ks. Very low-mass M dwarfs show a distinct drop in X-ray luminosity compared to slightly more massive M dwarfs. Surprisingly, this does not happen at the mass threshold where M dwarfs become fully convective (M4), but at significantly lower masses (M8). These very low mass stars seem to have a flaring behaviour different from earlier type stars: they display either occasional large flares or a very low-level "flickering" in their X-ray light curves, but not the canonical power-law flare-energy distribution observed for the Sun and other cool stars. Our aim is to collect a long-duration light curve for one of the most nearby ultracool dwarfs to quantify how its flare-energy distribution differs from earlier type stars.

X-ray driven evaporation of exoplanet atmospheres: discovery of a uniquely suited test system

The evaporation of exoplanetary atmospheres is thought to be driven by high-energy irradiation. However, the actual mass loss rates are not well constrained. Co-I Kipping has recently discovered that the star KOI-314, an M1V dwarf at 65 pc distance, is orbited by two earth-sized planets, the inner one of them rocky and the outer one gaseous (P_orb = 14d and 23d). Other recent works have shown an abundance of small rocky planets in very close orbits around their host stars, suggesting that the stellar high-energy irradiation evaporates away gaseous envelopes. KOI-314 is the first nearby system in which earth-sized planets of both types are detected, allowing us to constrain the efficiency of planetary evaporation if the stellar X-ray irradiation is measured. We therefore propose a 10 ks Chandra ACIS-S pointing to determine the stellar X-ray luminosity and hardness ratio. The accuracy of the orbital solution decreases quickly due to Transit-Timing Variations, which is why we ask for DDT.

The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems

When a planet transits its host star, it blocks regions of the stellar surface from view; this causes a distortion of the spectral lines and a change in the line-of-sight (LOS) velocities, known as the Rossiter-McLaughlin (RM) effect. Since the LOS velocities depend, in part, on the stellar rotation, the RM waveform is sensitive to the star-planet alignment (which provides information on the system’s dynamical history). We present a new RM modelling technique that directly measures the spatially-resolved stellar spectrum behind the planet. This is done by scaling the continuum flux of the (HARPS) spectra by the transit light curve, and then subtracting the infrom the out-of-transit spectra to isolate the starlight behind the planet. This technique does not assume any shape for the intrinsic local profiles. In it, we also allow for differential stellar rotation and centre-to-limb variations in the convective blueshift. We apply this technique to HD 189733 and compare to 3D magnetohydrodynamic (MHD) simulations. We reject rigid body rotation with high confidence (>99% probability), which allows us to determine the occulted stellar latitudes and measure the stellar inclination. In turn, we determine both the sky-projected (λ ≈ −0.4 ± 0.2◦) and true 3D obliquity (ψ ≈ 7+12 −4 ◦ ). We also find good agreement with the MHD simulations, with no significant centre-to-limb variations detectable in the local profiles. Hence, this technique provides a new powerful tool that can probe stellar photospheres, differential rotation, determine 3D obliquities, and remove sky-projection biases in planet migration theories. This technique can be implemented with existing instrumentation, but will become even more powerful with the next generation of high-precision radial velocity spectrographs.

Modeling the Rossiter-McLaughlin Effect: Impact of the Convective Center-to-limb Variations in the Stellar Photosphere

bservations of the Rossiter–McLaughlin (RM) effect provide information on star–planet alignments, which can inform planetary migration and evolution theories. Here, we go beyond the classical RM modeling and explore the impact of a convective blueshift that varies across the stellar disk and non-Gaussian stellar photospheric profiles. We simulated an aligned hot Jupiter with a four-day orbit about a Sun-like star and injected center-to-limb velocity (and profile shape) variations based on radiative 3D magnetohydrodynamic simulations of solar surface convection. The residuals between our modeling and classical RM modeling were dependent on the intrinsic profile width and v sin i; the amplitude of the residuals increased with increasing v sin i and with decreasing intrinsic profile width. For slowly rotating stars the center-to-limb convective variation dominated the residuals (with amplitudes of 10 s of cm s−1 to ~1 m s−1); however, for faster rotating stars the dominant residual signature was due a non-Gaussian intrinsic profile (with amplitudes from 0.5 to 9 m s−1). When the impact factor was 0, neglecting to account for the convective center-to-limb variation led to an uncertainty in the obliquity of ~10°–20°, even though the true v sin i was known. Additionally, neglecting to properly model an asymmetric intrinsic profile had a greater impact for more rapidly rotating stars (e.g., v sin i = 6 km s−1) and caused systematic errors on the order of ~20° in the measured obliquities. Hence, neglecting the impact of stellar surface convection may bias star–planet alignment measurements and consequently theories on planetary migration and evolution.

Ultraviolet emission lines of Si II in cool star and solar spectra

Recent atomic physics calculations for Si II are employed within the CLOUDY modelling code to analyse Hubble Space Telescope (HST) STIS ultraviolet spectra of three cool stars, β Geminorum, α Centauri A and B, as well as previously published HST/GHRS observations of α Tau, plus solar quiet Sun data from the High Resolution Telescope and Spectrograph. Discrepancies found previously between theory and observation for line intensity ratios involving the 3s²3p ²PJ-3s3p^{2 4}P^J' intercombination multiplet of Si II at ~ 2335 Å are significantly reduced, as are those for ratios containing the 3s²3p ²PJ-3s3p^{2 2}DJ ~ transitions at ~1816 Å. This is primarily due to the effect of the new Si II transition probabilities. However, these atomic data are not only very different from previous calculations, but also show large disagreements with measurements, specifically those of Calamai et al. for the intercombination lines. New measurements of transition probabilities for Si II are hence urgently required to confirm (or otherwise) the accuracy of the recently calculated values. If the new calculations are confirmed, then a long-standing discrepancy between theory and observation will have finally been resolved. However, if the older measurements are found to be correct, then the agreement between theory and observation is simply a coincidence and the existing discrepancies remain.

M Dwarf Flare Continuum Variations on One-second Timescales: Calibrating and Modeling of ULTRACAM Flare Color Indices

We present a large data set of high-cadence dMe flare light curves obtained with custom continuum filters on the triple-beam, high-speed camera system ULTRACAM. The measurements provide constraints for models of the near-ultraviolet (NUV) and optical continuum spectral evolution on timescales of ≈1 s. We provide a robust interpretation of the flare emission in the ULTRACAM filters using simultaneously obtained low-resolution spectra during two moderate-sized flares in the dM4.5e star YZ CMi. By avoiding the spectral complexity within the broadband Johnson filters, the ULTRACAM filters are shown to characterize bona fide continuum emission in the NUV, blue, and red wavelength regimes. The NUV/blue flux ratio in flares is equivalent to a Balmer jump ratio, and the blue/red flux ratio provides an estimate for the color temperature of the optical continuum emission. We present a new “color-color” relationship for these continuum flux ratios at the peaks of the flares. Using the RADYN and RH codes, we interpret the ULTRACAM filter emission using the dominant emission processes from a radiative-hydrodynamic flare model with a high nonthermal electron beam flux, which explains a hot, T ≈ 104 K, color temperature at blue-to-red optical wavelengths and a small Balmer jump ratio as observed in moderate-sized and large flares alike. We also discuss the high time resolution, high signal-to-noise continuum color variations observed in YZ CMi during a giant flare, which increased the NUV flux from this star by over a factor of 100. Based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium, based on observations made with the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, and observations, and based on observations made with the ESO Telescopes at the La Silla Paranal Observatory under programme ID 085.D-0501(A).

Unraveling the Dust Formation Process in R Dor

Using both dynamical and chemical modelling, we derive an accurate abundance profile for the molecule SiO in the stellar wind of R Dor, an O-rich AGB star. SiO plays a key role in the dust formation process in O-rich AGB stars. This method will be applied to additional molecules, with the aim to achieve a detailed overview of the molecular abundance pattern in the wind of R Dor.

Chromatic Aberration

Chromatic Aberration is a film installation which explores the early technologies of colour filmmaking drawn from the archives of George Eastman House, Rochester, New York. Featuring vibrant close-ups of eyes from fledgling archival experiments in colour film, Chromatic Aberration turns the cinematic lens in on itself: from the prosthetic recording eye of the camera, to an evocation of the abstract inner screen of one's eyelids. Early 1920s colour film footage - mainly tests shots featuring members of George Eastman's family as well as Hollywood stars of the time - is shot in such a way so as to reveal the inherent chromatic fringing, distortion and misalignment. Using specialist equipment at the BFI National Archive, London, the footage is reworked through the use of extreme close-up and magnification, honing in on the eyes. The installation evokes an imagined abstract colour world, a flickering eyelid trapped in a mechanical peephole. Exhibitions: Solo exhibition as film installation at Tyneside Cinema (Newcastle, Oct-Nov 2014); Solo exhibition at George Eastman Museum (Rochester, New York, Jan-April 2015), including a second work on display. Film festivals nominations for competitions: Winner of Best Vanguard Film Competition in Lima Independiente International Film Festival (Peru). Nominations: Filmadrid festival (Spain); Curtas Vila do Conde film festival (Portugal); Festival du Nouveau Cinema (Canada); Jihlava International Documentary Film Festival (Czech Republic ); International Film Festival Bratislava (Slovenia). Additional screenings at International Rotterdam Film Festival (Netherlands); European Media Art Festival (Germany); BFI London Film Festival (UK); Mini-retrospective screening at DIM CINEMA, The Cinematheque (Vancouver May 2015). Reviews and interviews in Artforum, The Wire Magazine, After Image, Studio International. Public lectures: with Prof. Sarah Street at Tyneside Cinema (Nov 2014); Royal Academy visiting public lecture (Nov 2014); ‘The Laughter of Things’ symposium, International Film Festival Rotterdam and Piet Zwart Institute (Jan 2015); George Eastman Museum and Rochester University (April 2015). Acquired by the George Eastman Museum for their collection.

Modos r de oscilação em estrelas de neutrões

Tese dout., Física - Astrofísica, Universidade do Algarve, 2007

Beach quality assessment and management in the Sotavento (Eastern) Algarve, Portugal

The purpose of this study on beach quality assessment and management was to evaluate the quality of five beaches in the Algarve Sotavento region of Portugal and to identify beach users’ preferences and priorities regarding their visit to a beach. The Algarve is one of the country’s most internationally known regions and it is generally perceived as a major tourist destination. Because of the increasing level of tourists, there is a specific need to address beach quality, as overcrowding can result in excessive litter, reduce water quality and consequently reduce the socio-economic value of the area. The main methodology for the evaluation of the beach quality in this pilot project was the Bathing Area Registration and Evaluation framework (BARE), which recognizes five beach types (rural, remote, resort, urban and village) through five main priority issues of concern to beach users (water quality, scenery, litter, safety, facilities) and evaluates the beach quality, ranging from one (low) to five (high) stars. After overall bathing area classification, Quarteira-Vilamoura, Ilha do Farol, Ilha Deserta and Ilha da Armona received three-star rating and Quinta do Lago site obtained a one-star rating. The quantitative research data on beach users’ preferences and priorities was obtained through administration of 50 questionnaires per beach and showed that beach users at all sites expressed the need for improved cleanliness, safety and facilities on the beach. The BARE framework, together with the questionnaire surveys, allowed the identification of management priorities required to improve the quality of individual beaches and therefore increase income from tourism.

Crieff Hydro Hotel: the experience economy and the guest perspective

The purpose of this report is to do a presentation of the hotel where I will be working, characterising the reception department and all the activities that I developed during this placement. On this placement at the CHH (Crieff Hydro Hotel) – family 4 stars resort, my goal is to have an experience in hospitality, in special in reception. This placement is carried out from my Master degree in Direcção e Gestão Hoteleira (Commercial branch) at the University of the Algarve – Campus Penha. For this report it was also intended to do an analysis of the guest experience in hospitality and for that it was necessary to do a literature review adequate for my area of work in the hotel giving importance to the guest experience in the hospitality. For my analysis regarding the guest experience in hospitality, I used data collected from the surveys answered by the guests that stayed with us in the hotel. To analyse the data it was necessary to do a categorial analysis technique. After this year of placement in the hotel and after this analysis, as results I have the opportunity to continue my work in the hotel and also the possibility of a better position in a near future. Last but not least, this report demonstrates my work path and also helps to have a better understanding of the satisfaction perceived by the guest in order to give us tools to improve it. From what we can see, the guests’ satisfaction is highly rated on both surveys.

Guest reputation indexes to analyze hotel’s online reputation using data extracted from OTAs

Nowadays many travelers use online travel agency (OTAs) to book flights, hotel rooms, rent-a-cars, cruises or entire vacation packages. Usually OTAs allow their users to give scores and to write reviews about what was used. Each OTA defines the terms and conditions for guest rating or review score and hoteliers are giving increasing importance to the scores and reviews their guests do in OTAs. This paper proposes two guest reputation index to help hoteliers to monitorize their presence in OTAs. The Aggregated Guest Reputation Index (AGRI), which shows the positioning of a hotel in different OTAs and it is calculated from the scores obtained by the hotels in those OTAs. Another one, the Semantic Guest Reputation Index (SGRI), which incorporates the social reputation of a hotel and that can be visualized through the development of word clouds or tag clouds. Examples of usage of these indexes are given with data extracted from 5-stars hotels in the Algarve, south region of Portugal, that are available on Booking and Expedia.

Vom Trümmerfilm zur Traumfabrik : die "Junge Film-Union". Eine Fallstudie zur westdeutschen Filmproduktion

Die Trümmer des deutschen Reiches waren 1945 auch die Trümmer des deutschen Films. Der Neuaufbau der deutschen Filmwirtschaft, der unter der Ägide der Alliierten begann, eröffnete trotz zahlloser Schwierigkeiten neue Chancen, nicht zuletzt regional: auch Niedersachsen wurde "Filmland". Die "Junge Film-Union", 1947 lizensiert, wurde bald zur größten niedersächsischen Filmproduktionsfirma. Waren die ersten zeitnahen Filme - auch "Trümmerfilme" genannt - noch in mancher Hinsicht improvisiert, so professionalisierte sich die Produktion zusehends. Es wurden eigene Ateliers gebaut, in dem Heideort Bendestorf entstand in kurzer Zeit eine Filmindustrie. Und auch die Filmstoffe wandelten sich, ebenso die Besetzung der Hauptrollen: der "zeitlose" Unterhaltungsfilm wurde selbstverständlich, ein neuer Kult mit alten Stars verdrängte den Nachwuchs. Neben vielen Mißerfolgen der "Jungen Film-Union" wurde schließlich "Die Sünderin" zu einem (Skandal-)Erfolg, der Marika-Rökk-Film "Die Csardas-Fürstin" ein echter Publikumsrenner. Der spektakuläre Neuaufbau dieser Filmproduktion, die wechselvolle Entwicklung, die im Konkurs 1952 ein jähes Ende fand, werfen Fragen auf, denen in dieser Arbeit auf der Basis neuen Quellenmaterials nachgegangen wird. Welche politischen, ökonomischen und kulturellen Einflüsse waren es, die für die "Junge Film-Union" bestimmend wurden. Welche Rolle spielte die britische Filmpolitik? Welche Bedeutung hatte die Währungsreform, wie wirkten sich die Bundesbürgschaften aus? Welche filmischen Traditionen wurden aufgegriffen, und wie spiegelt sich die außerfilmische Realität in den Produktionen? Die Ergebnisse der Untersuchung werfen dabei auch ein Licht auf den Neuaufbau der westdeutschen Filmwirtschaft insgesamt.