Interruptions Produced by the Mollucan Students in the Fellowship Meeting

This thesis is about a study of the interruptions produced by the Moluccan students in a fellowship meeting, consisting of fifteen students as the respondents, who are divided into two: the chairperson and the members. The purposes of the study are to know the tokens and the functions of interruptions used by the chairperson and the members of the meeting by considering social role as the social factor. The writer applies the theory of interruptions by Tannen (1990) and Wardhaugh (1985) as the main theories. Besides, the writer also uses the theory of social role by Johnstone (2008) and the theory of discourse markers by Schiffrin (2003) as the supporting theories. The writer used qualitative approach to conduct this research. The writer discovered that the chairperson produced more tokens (19) than the members (13). Moreover, the writer found that the respondents produced Ambonese tokens, such as “Hiii”, “Weee”, “Seng”, “Eee”, and Suroboyoan tokens, such as “Lho” and “Itulho”. Both the chairperson and the members produced “other” functions the most with 58.75% and 63.81%. In conclusion, social role influenced the interruptions and their functions, and the number of tokens produced by the participants

Star Cluster Formation and Disruption Time-Scales - II. Evolution of the Star Cluster System in M82's Fossil Starburst

ABRIDGED: We obtain new age and mass estimates for the star clusters in M82's fossil starburst region B, based on improved fitting methods. Our new age estimates confirm the peak in the age histogram attributed to the last tidal encounter with M81; we find a peak formation epoch at slightly older ages than previously published, log(t_peak / yr) = 9.04, with a Gaussian sigma of Delta log(t_width) = 0.273. Cluster disruption has removed a large fraction of the older clusters. Adopting the expression for the cluster disruption time-scale of t_dis(M)= t_dis^4 (M/10^4 Msun)^gamma with gamma = 0.62 (Paper I), we find that the ratios between the real cluster formation rates in the pre-burst phase (log(t/yr) <= 9.4), the burst-phase (8.4 < log(t/yr) < 9.4) and the post-burst phase (log(t/yr) <= 8.4) are about 1:2:1/40. The mass distribution of the clusters formed during the burst shows a turnover at log(M_cl/Msun) ~ 5.3 which is not caused by selection effects. This distribution can be explained by cluster formation with an initial power-law mass function of slope alpha=2 up to a maximum cluster mass of M_max = 3 x 10^6 Msun, and cluster disruption with a normalisation time-scale t_dis^4 / t_burst = (3.0 +/- 0.3) x 10^{-2}. For a burst age of 1 x 10^9 yr, we find that the disruption time-scale of a cluster of 10^4 Msun is t_dis^4 ~ 3 x 10^7 years, with an uncertainty of approximately a factor of two. This is the shortest disruption time-scale known in any galaxy.Comment: 14 pages including 8 postscript figures; accepted for publication in MNRA

The Hanbury Brown and Twiss Experiment with Fermions

We realized an equivalent Hanbury Brown and Twiss experiment for a beam of electrons in a two dimensional electron gas in the quantum Hall regime. A metallic split gate serves as a tunable beam splitter which is used to partition the incident beam into transmitted and reflected partial beams. The current fluctuations in the reflected and transmitted beam are fully anticorrelated demonstrating that fermions tend to exclude each other (anti-bunching). If the occupation probability of the incident beam is lowered by an additional gate, the anticorrelation is reduced and disappears in the classical limit of a highly diluted beam

N-body simulations of star clusters

Two aspects of our recent N-body studies of star clusters are presented: (1) What impact does mass segregation and selective mass loss have on integrated photometry? (2) How well compare results from N-body simulations using NBODY4 and STARLAB/KIRA?Comment: 2 pages, 1 figure with 4 panels (in colour, not well visible in black-and-white; figures screwed in PDF version, ok in postscript; to see further details get the paper source). Conference proceedings for IAUS246 'Dynamical Evolution of Dense Stellar Systems', ed. E. Vesperini (Chief Editor), M. Giersz, A. Sills, Capri, Sept. 2007; v2: references correcte

Analisis Unsur Manajemen dalam Pengolahan Rekam Medis di Rumah Sakit TNI AU Lanud Roesmin Nurjadin

Hospitals must conduct a medical record activities according to Permenkes NO.269 / MENKES / PER / III / 2008 about Medical Record, to achieve the purpose of medical record processing required 5 management elements are: man, money, material, machine, and method. The medical record processing that has been implemented at the Hospital TNI AU LANUD Roesmin Nurjadin that is coding, coding only done for BPJS patients whose conducted by the officer with education background of D3 nursing, it be impacted to the storage part is wrong save and cannot found patient medical record file because are not returned. The purpose of this research is to know the element of management in the processing of medical records at the Hospital TNI AU LANUD Roesmin Nurjadin. This research is done by Qualitative descriptive method, Qualitative approach, instrument of data collection of interview guidance, observation guidance, check list register, and stationery, number of informant 6 people with inductive way data analysis. The result of this research found that Mans elements only amounts to 2 people so that officers work concurrently and have never attended training, material element and machines elements of medical record processing not yet use SIMRS and tracer, while processing method elements follow existing habits and follow the policy of hospital that is POP organization. Keywords: Management elements, medical record processin

On the nature of the bi-stability jump in the winds of early-type supergiants

We study the origin of the observed bi-stability jump in the terminal velocity of the winds of supergiants near spectral type B1. To this purpose, we have calculated a grid of wind models and mass-loss rates for these stars. The models show that the mass-loss rate 'jumps' by a factor of five around spectral type B1. Up to now, a theoretical explanation of the observed bi-stability jump was not yet provided by radiation driven wind theory. The models demonstrate that the subsonic part of the wind is dominated by the line acceleration due to Fe. The elements C, N and O are important line drivers in the supersonic part of the wind. We demonstrate that the mass-loss rate 'jumps' due to an increase in the line acceleration of Fe III below the sonic point. Finally, we discuss the possible role of the bi-stability jump on the mass loss during typical variations of Luminous Blue Variable stars.Comment: Accepted by A&A, 19 pages Latex, 10 figure