By February 24, 2014 Read More →

Ambiance for Android

App Name: Ambiance

Cost: $2.99 USD

DeveloperUrban Apps

MarketGoogle Play

Review: Having a tough day? Want to relax and just unwind some? One of the best way to change your mood is by what you listen to.  The Ambiance app for Android does just that. You can create your own library of relaxing and soothing sounds which you can play any time you need a change. You can choose from over 2500 free sounds, exclusive to Ambiance, to download and create your customized sound mixes.

The app has a lot of nice features and a number of features that will be coming out in future updates. When looking for a particular sound you can search the store by categories or keywords. You can preview any sound before downloading it. Within the library you will have a list of the files you downloaded and you can create mixes and playlists.

With the copy I reviewed the alarm, quickstart, backup, and recorder features were not working but I bet you can figure out what each of these will do.

Check out their intro video here

Overall the app is a very easy way to create your own library of soothing and relaxing sounds. I found using the headphone with the app was best to really hear the ocean waves or the early morning bird calls. So you are looking for a way to help block out a lot of the noise of your day, give Ambiance a try.

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  4. Full text disponibile come:2622KbAbstract (inglese)Dark matter (DM) is the dominant mass component in the universe and also the major constituent of cosmological structures like galaxy clusters or galaxies. Therefore, dark matter plays a fundamental role in the formation and evolution of these structures. During the past decades, the formation, dynamics and evolution of the DM halos, has been studied in great detail. The outcome of all the cosmological simulations is that the dissipationless DM component forms a nearly stable halo with an almost universal density shape, which is well fitted by the profile given by Navarro et al. (1997, hereafter NFW). However, the density profiles derived from the observed rotation curves of spiral galaxies (in particular, from Low Surface Bright galaxies) show much shallower profiles than the NFW profile or even indicate a core structure. Moreover theoretical considerations based on Jeans equation give a message of the same sign. Therefore, the question arises whether the DM halo profiles really have an universal shape and, in particular, which mechanisms or processes could then influence or change the DM density profile towards the observed ones. The Dynamical Theory of Clausius Virial (TCV) of Secco (2005) represents an interesting way to attack it starting from the exsistence of the galaxy Fundamental Plane (FP). This theory moves from the fact that a two component system, built up of a stellar spheroid completly embedded in a massive dark matter halo, may reaches a maximum amount of virial potential energy, called Clausius Virial (CV), related to its bright component. This is unexpected with respect of the monotonic behavior of its corresponding total potential energy. This is of extreme interest, as every time a stationary point appears in a dynamical quantity of a mechanical system, it may be a special configuration for the system. The existence of a maximum in the CV could be a sort of dynamical ”attractor”, a reference point for the galaxy structure. The first version of the theory was formulated by using two power laws for the mass density profiles of the two component. Inspite of its semplicity, it allowed detailed and especially analytical analysis of the main mechanisms intervening in the CV maximization. Moreover it was able to explain some of the most important scaling relations of early type galaxies (ETGs) as soon as the inner slope of DM density profile was lower than 1. As further step we extend here this analysis to more complex and realistic descriptions of real ETGs. The twofold aim of this thesis is then: (i) to produce a new TCV approach with more realistic and self consistent dynamical models of ETGs in order to analyze if stationary points are present, what are their follow up on the features of FP; (ii) to understand how these outputs of TCV are linked to the value of the inner slope of the DM halo and to cosmology. In the present new, higher level of approximation the TCV is developed modelling the stellar component by a King model with a cut off. The inner component is now more realistic for the ETGs even if the DM halo density remains a cored power law. In this framework again a maximum value for the Clausius’ virial energy (CV) of the baryonic component exists, and the corresponding configuration has the property to share its virial energy into two parts: one due to the self gravity of baryons and the other one to the fraction of dark matter (DM) which exerts dynamical effects on the first. In order to do that, the new TCV approach needs to be strictly linked to the cosmology. The partial degeneracy of FP with respect to the initial density perturbation spectrum, underlined firstly by Djorgovski (1992), may be now fully understood in a CDM cosmological scenario. (1997) in B band, give us more prompts about the slope. From the outputs of this theory the FP coefficients for the ETGs so as the trend mass/luminosity vs. mass (the tilt) are fairly good reproduced if the bulk of baryons are embedded into a DM universal density profile around . Under this condition, also the ZOE may be explained. In this case, the ZOE limit appears to be bent in the galaxy mass range and reaches that found by Burstein et al. (1997) only when the masses become of the order of the Galaxy Clusters. The slope relevance is also correlated with the attractiveness of CV maxima which is in turn linked to the thermodynamical properties of CV maxima. Inside this framework we have explored the fate for collisionless systems when a violent mechanism acts to lead them to virial equilibrium. In order to justify the link of the mean temperature of the stellar component to the kinetic energy of the component, assumed in TCV as an ansatz, we need to know if, on the classical basis, we are dealing at the end of the relaxation phase with a unique Gaussian for this star mixture, or not. The thermodynamical non linear approach of the TCV, we have also performed in a preliminary way, shows that the comparison between the CV maxima inside a and inside a NFW profile, tells us that when they are present in this last case, they do not work as attractors of the relaxed configuration of the baryons as in the previous case.

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