Signs Of Youth Research Articles

Jawline Sharp Contouring With Hybrid Filler.

Having a well-defined jawline is a sign of youth and attractiveness among both men and women. Soft tissue fillers, such as calcium hydroxylapatite (CaHA) and hyaluronic acid (HA) fillers, offer nonsurgical alternatives for rejuvenating the lower face and enhancing the jawline. The aim of this study was to investigate the use of a premixed combination of HA with cohesive polydensified matrix technology (CPM, Belotero Intense, CPM-I) and CaHA to create a sharply defined jawline. A total of 126 patients were enrolled in the study and treated with a premixed combination of CPM-I and CaHA using a retrograde fanning injection technique with cannulas. The injection volumes and product ratios were customized according to the patients' needs. The cohort consisted of 75 females and 51 males. The average injected volume of premixed CaHA:CPM-I was 5.83mL. In the majority of patients, a 1:1 syringe ratio of CaHA:CPM-I was applied (n = 81, 64.2%). No adverse events were reported during the 6-month follow-up period. The hybrid filler approach investigated in this study shows promise for achieving well-defined, long-lasting jawline contours. This journal requires that authors assign a level of evidence to each article. For a full description of these Evidence-Based Medicine ratings, please refer to the Table of Contents or the online Instructions to Authors www.springer.com/00266 .

Clinical and practical aspects of the gingival smile. A questionnaire-based survey.

Abstract Introduction: One of the main elements of facial esthetics is represented by the smile. A harmonious proportion between the elements of facial esthetics is an important subject of interest in dentistry. Aim of the study: This research aims to evaluate the impact of the gummy smile on future dental practitioners. Materials and Methods: A survey containing 16 questions was designed to find out the students’ perceptions about the ideal smile and if the gingival smile is considered youthful or unpleasing. The impact on their self-esteem, their willingness to change the gummy smile or not, the nonsurgical and surgical methods of treatment were also evaluated. Results: 212 answers were recorded and analyzed. Nearly three quarters (70.3%) of the respondents believe that having a gummy smile is unesthetic, while only 29.3% considered it to be a sign of youth. Self-esteem can be affected by having a gingival smile, but, according to the results, most of the students (45.8%) said that their daily lives have not been affected by it, 40.6% said that in a small amount, 10.4% said that their self-assurance has been very affected and only 3.3% admitted that the gummy smile distressed their confidence. When asked if they were willing to correct their gingival smile, 51.4% were open to improving it while 48.6% would not change it. Conclusions: Among dentistry students, excessive showing of the gums is believed to be unesthetic rather than a sign of youthfulness. The respondents are generally not affected in their daily life by having a gummy smile. Education regarding the methods of correcting it still needs to be addressed amongst future dental practitioners.

Characterising young visual M-dwarf binaries with near-infrared integral field spectra

We present the results from an integral field spectroscopy study of seven close visual binary pairs of young M-dwarf multiple systems. The target systems are part of the astrometric monitoring AstraLux programme, surveying hundreds of M-dwarf systems for multiplicity and obtaining astrometric epochs for orbital constraints. Our new VLT/SINFONI data provides resolved spectral type classifications in the J, H, and K bands for seven of these low-mass M-dwarf binaries, which we determine by comparing them to empirical templates and examining the strength of water absorption in the K band. The medium resolution K-band spectra also allows us to derive effective temperatures for the individual components. All targets in the survey display several signs of youth, and some have kinematics similar to young moving groups, or low surface gravities which we determined from measuring equivalent widths of gravity sensitive alkali lines in the J band. Resolved photometry from our targets is also compared with isochrones from theoretical evolutionary models, further implying young ages. Dynamical masses will be provided from continued monitoring of these systems, which can be seen as emblematic binary benchmarks that may be used to calibrate evolutionary models for low-mass stars in the future.

Irregular Dust Features around Intermediate-mass Young Stars with GPI: Signs of Youth or Misaligned Disks?

Abstract We are undertaking a large survey of over 30 disks using the Gemini Planet Imager (GPI) to see whether the observed dust structures match spectral energy distribution predictions and have any correlation with stellar properties. GPI can observe near-infrared light scattered from dust in circumstellar environments using high-resolution Polarimetric Differential Imaging with coronagraphy and adaptive optics. The data have been taken in the J and H bands over two years, with inner working angles of 0.″08 and 0.″11, respectively. Ahead of the release of the complete survey results, here we present five objects with extended and irregular dust structures within 2″ of the central star. These objects are FU Ori, MWC 789, HD 45677, Hen 3-365, and HD 139614. The observed structures are consistent with each object being a pre-main-sequence star with protoplanetary dust. The five objects’ circumstellar environments could result from extreme youth and complex initial conditions, from asymmetric scattering patterns due to shadows cast by misaligned disks, or in some cases from interactions with companions. We see complex U ϕ structures in most objects that could indicate multiple scattering or result from the illumination of companions. Specific key findings include the first high-contrast observation of MWC 789 revealing a newly discovered companion candidate and arc, and two faint companion candidates around Hen 3-365. These two objects should be observed further to confirm whether the companion candidates are comoving. Further observations and modeling are required to determine the causes of the structures.

β PICTORIS AND AB DORADUS MOVING GROUPS: LIKELY NEW LOW-MASS MEMBERS

We present results from our continuing program to identify new, low-mass, members of the nearby young moving groups (NYMGs) using a proper motion selection algorithm and various observational techniques. We have three goals: 1) To provide high priority targets for exoplanet searches by direct imaging, 2) To complete the census of the membership in the NYMGs down to ~0.1 Msun, and thus 3) Provide a well-characterized sample of nearby (median distances at least twice as close as the Taurus and Ophiuchus SFR's), young (8-50 Myr) stars for detailed study of their physical properties and multiplicity. Our program proceeds as follows: we apply the selection algorithm to a proper motion catalog where initial selection cuts of candidate members are based on the mean motion of known NYMG members and the proper motions and photometric distances of the candidates. NYMG membership is investigated further using possible signs of youth, including H-alpha emission and X-ray flux, and then verified through radial velocity (RV) measurements. We identify TYC 1766-1431-1 (M3), TYC 1208-468-1 and 2 (K3), TYC 7558-655-1 (K5), and PM I04439+3723W and E (M3) as likely members of the Beta Pictoris moving group (BPMG) and TYC 1741-2117-1N and S (K7), TYC 1752-63-1 (K7), TYC 523-573-1 (K7), and TYC 4943-192-1 (M0) as likely members of the AB Doradus moving group (ABDMG). We also rule out the membership of several BPMG and ABDMG candidates. To date our program has identified 16 new NYMG members of spectral type K3 or later.

Treatment of alopecia by transplantation of hair follicle stem cells and dermal papilla cells encapsulated in alginate gels

The affected individual of hair loss demands help, because hair is viewed as a sign of youth and good health. Nowadays treatment of alopecia includes drug therapy and hair transplantation. Some drugs may promote hair growth, at least temporarily, but the treatment is effective only in milder alopecia, instead of extensive alopecia. Furthermore, the side effect of long period medication could not be avoided. Hair transplantation involves harvesting small pieces of hair-bearing scalp grafts from a donor site and relocating them to a bald area. This method does not increase the number of existing hairs, but only redistributes them. The operation is sophisticated and time-consuming, thus the patient suffers a lot during the process. The discovery of hair follicle stem cells (FSC) brings gospel to the affected individual of hair loss because of its capacity of generating new hair when they interact with mesenchymal dermal papilla cells (DPC). Besides, both FSC and DPC have strong proliferative capacity and the patient's own cells could be expanded considerably in vitro. Thus we hypothesize that the microencapsulation of the two kinds of cells in alginate gels could be implanted into the bald scalp of the patient since alginate gels is effective in cell transplantation. The strategy may provide a more convenient and valid alternative to hair loss if the hypothesis proved to be practical.

Compact radio sources and jet-driven AGN feedback in the early universe: constraints from integral-field spectroscopy

To investigate the impact of radio jets during the formation epoch of their massive host galaxies, we present an analysis of two massive, log M{sub stellar}/M{sub {circle_dot}} {approx} 10.6 and 11.3, compact radio galaxies at z = 3.5, TNJ0205+2242 and TNJ0121+1320. Their small radio sizes (R {le} 10 kpc) are most likely a sign of youth. In particular, we compare their radio properties and gas dynamics with those in well extended radio galaxies at high redshift, which show strong evidence for powerful, jet-driven outflows of significant gas masses (M {approx} 10{sup 9-10} M{sub {circle_dot}}). Our analysis combines rest-frame optical integral-field spectroscopy obtained with SINFONI on the VLT with existing radio imaging, CO(4-3) emission line spectra, and rest-frame UV longslit spectroscopy. [OIII]{lambda}5007 line emission is compact in both galaxies and lies within the region defined by the radio lobes. For TNJ0205+2242, the Ly{alpha} profile narrows significantly outside the jet radius, indicating the presence of a quiescent halo. TNJ0121+1320 has two components at a projected relative distance of {approx}10 kpc and a velocity offset of {approx}300 km s{sup -1}, measured from the [OIII]{lambda}5007 velocity map. This suggests that the fainter component is orbiting around the more massive, radio-loud galaxy. If motions aremore » gravitational, this implies a dynamical mass of 2 x 10{sup 11} M{sub {circle_dot}} for the radio-loud component. The dynamical mass, molecular gas mass measured from the CO line emission, and radio luminosity of these two compact radio galaxies imply that compact radio sources may well develop large-scale, energetic outflows as observed in extended radio galaxies, with the potential of removing significant fractions of the ISM from the host galaxy. The absence of luminous emission line gas extending beyond the radio emission in these sources agrees with the observed timescales and outflow rates in extended radio galaxies, and adds further evidence that the energetic, large-scale outflows observed in extended radio sources (Nesvadba et al. 2006) are indeed the result of influence of the radio jet.« less

Unraveling the Origins of Nearby Young Stars

A systematic search for close conjunctions and clusterings in the past of nearby stars younger than the Pleiades is undertaken, which may reveal the time, location, and mechanism of formation of these often isolated, disconnected from clusters and star-forming regions, objects. The sample under investigation includes 101 T Tauri, post-TT, and main-sequence stars and stellar systems with signs of youth, culled from the literature. Their Galactic orbits are traced back in time and near approaches are evaluated in time, distance, and relative velocity. Numerous clustering events are detected, providing clues to the origin of very young, isolated stars. Each star's orbit is also matched with those of nearby young open clusters, OB and TT associations and star-forming molecular clouds, including the Ophiuchus, Lupus, Corona Australis, and Chamaeleon regions. Ejection of young stars from open clusters is ruled out for nearly all investigated objects, but the nearest OB associations in Scorpius-Centaurus, and especially, the dense clouds in Ophiuchus and Corona Australis have likely played a major role in the generation of the local streams (TWA, Beta Pic, and Tucana-Horologium) that happen to be close to the Sun today. The core of the Tucana-Horologium association probably originated from the vicinity of the Upper Scorpius association 28 Myr ago. A few proposed members of the AB Dor moving group were in conjunction with the coeval Cepheus OB6 association 38 Myr ago.

Herbig-Haro flows in L1641N

Mass is clearly the most important parameter of a star as it determines the phases it will go through, its physical parameters, the elements produced and its life span. Two important processes that occur simultaneously in young stars are directly related to the final mass a star ends up with; the accretion of material onto the star from a circumstellar disk and the bipolar outflow of material from the star. These processes are related since the infalling material drives the outflow. The life span of circumstellar disks is also important for the possibility of life, as this limits the time available for planet formation. This may depend on the stellar mass and its environment.Three detailed observational case-studies are presented, a globule (B335) that is forming only one or two stars, a medium-sized star formation region (L1551) and a large cluster of young stars (YSOs) in a part of our nearest giant molecular cloud (L1641N).The first part of this thesis concerns finding YSOs by looking for mid-IR excess, indicative of circumstellar disks, using the ISO and Spitzer satellites in combination with ground-based observations. Other signs of youth are also used; H-alpha in emission (accretion), Li 6707 in absorption (Li is destroyed with age) and cloud membership based on extinction. The detection of 15 new YSO candidates in L1551 (Paper I) and 89 YSOs in L1641N (Paper II) is presented. In L1641N, distributions are presented of stellar age and mass. An empirical extinction law is found and the star formation history is presented. There seems to be an accelerated star formation with time. This can however also be explained, at least partly, by migration of older stars from the cluster - a migration that may very well be mass dependent.The second part concerns bipolar outflows. The discovery of six Herbig-Haro objects and at least 15 H2 objects in B335 is presented (Paper III) as well as proper motions for previously known objects. A planar shock model is used to calculate shock velocities. In L1641N (Paper IV) we discover a new outflow source and connect this to a number of H2 objects that are found to be part of this flow from proper motion measurements.

Search for new T Tauri stars in the Cepheus-Cassiopeia region

The Cepheus-Cassiopeia star-forming region has been searched for new T Tauri stars (TTSs) based on the ROSAT all sky survey (RASS). Optical spectroscopic observations were carried out toward 45 GSC stellar counterparts of RASS sources looking for the Li absorption line (6708 A), a sign of youth. The detection of this line resulted in finding 11 to 16 new TTSs in this region. Using follow-up optical photometric observations and evolutionary models these Li-rich stars are revealed to be young low-mass stars. The most of the young stars are separated from the $\element[][13]{CO}$ molecular clouds by ~10 pc, significantly more than in Chamaeleon. A group of the new TTSs are isolated from the CO clouds and distributed inside the previously determined CO void. Possible formation scenarios including the interaction with the supernova shock for the isolated TTSs are discussed.

Cheekbone: dynamic and anti-aging structure of the midface?

The cheekbone is not only a static structure but has also a dynamic function. The muscles responsible for its motions are generally ignored or poorly known because they have a tendency to disappear with aging. When present and trophic, they form recognized muscles such as the malaris muscle in the mid-cheek and the risorius muscle in the flabby cheek. These muscles enhance the muscular part of the superficial musculo-aponeurotic system (SMAS) and this has a dynamic effect on the cheek, e.g. the dimple. This article will attempt to demonstrate that the cheekbone could also be the dynamic consequence of a SMAS which is more muscular than aponeurotic, due to an involuntary mechanism whose neurological control is unconscious. Thanks to this, the cheekbone could have an anti-aging effect, since it determines the position of the mid-cheek. The malar bone is well-developed in African and Asian people, but is usually not so marked in Caucasians, although the malar prominence is generally considered to be a sign of youth and beauty. The classic Hellenic appearance shows this perfectly.