A Survey of Far Ultraviolet Spectroscopic Explorer Observations of Cataclysmic Variables

During its lifetime, the Far Ultraviolet Spectroscopic Explorer (FUSE) was used to observe 99 cataclysmic variables in 211 separate observations. Here, we present a survey of the moderate resolution (R\simeq10,000), far-ultraviolet (905 - 1188 {\deg}A), time-averaged FUSE spectra of cataclysmic variables (CVs). The FUSE spectra are morphologically diverse. They show contributions from the accretion disk, the disk chromosphere, disk outflows, and the white dwarf, but the relative contribution of each component varies widely as a function of CV subtype, orbital period and evolutionary state, inclination, mass accretion rate, and magnetic field strength of the white dwarf. The data reveal information about the structure, temperature, density and mass flow rates of the disk and disk winds, the temperature of the white dwarf and the effects of ongoing accretion on its structure, and the long-term response of the systems to disk outbursts. The complete atlas of time-averaged FUSE spectra of CVs are available at the Multimission Archive at Space Telescope Science Institute as a High Level Science Product.Comment: ApJS, in press. The extra panels in the figure sets for Figures 1 and 2 are included at the end of the manuscrip

Penerapan Teknik Permainan Dialog dalam Konseling Kelompok Gestalt untuk Mengurangi Tingkat Keterisolasian Siswa Kelas XI IPS di SMA Negeri 2 Pare

Berdasarkan hasil pengamatan dan wawancara di dapatkan fakta mengenai tingginya tingkat keterisolasian siswa di SMA Negeri 2 Pare. Hal ini di tunjukkan dengan adanya kasus siswa yang melamun di dalam kelas, sikap yang menutup diri, jarang berinteraksi dengan orang lain dan tidak bersemangat. Penelitian ini bertujuan untuk mengetahui perbedaan jumlah skor yang diperoleh siswa terisolasi sebelum dan sesudah diberikan teknik permainan dialog dalam konseling kelompok Gestalt pada kelas XI IPS di SMA Negeri 2 Pare. Subyek penelitian di ambil dari siswa kelas XI IPS, karena di harapkan mampu mengurangi tingkat keterisolasian siswa untuk memahami siapa dirinya dan bertanggung jawab atas perilakunya dan meningkatkan kebermaknaan hidupnya. Jenis penelitian ini adalah penelitian pre-eksperimental designs dengan jenis pre-test post-test one group design, sedangkan subyek penelitiannya adalah 9 siswa kelas XI IPS 1 dan IPS 2 di SMA Negeri 2 Pare yang memiliki tingkat keterisolasian tinggi. Metode yang digunakan untuk mengumpulkan data tentang siswa yang memiliki tingkat keterisolasian tinggi yakni dengan menggunakan angket. Teknik analisis data yang digunakan adalah Uji Tanda. Hasil analisis Uji Tanda menunjukkan bahwa tanda positif (+) berjumlah 9. Berarti N (banyaknya tanda yang lebih sedikit) adalah 9, sehingga X (banyaknya tanda yang lebih sedikit) adalah 0. Dengan melihat tabel tes binomial dengan ketentuan N=6 dan X=0, maka diperoleh ρ=0,002. Bila menggunakan ketetapan α (taraf kesalahan) sebesar 5% adalah 0,05 maka dapat di simpulkan bahwa harga 0,002 < 0,05, dengan demikian Ho di tolak dan Ha diterima. Hal ini membuktikan bahwa ada perbedaan jumlah skor yang di peroleh siswa terisolasi sesudah diberikan teknik permainan dialog dalam konseling kelompok Gestalt pada siswa kelas XI IPS di SMA Negeri 2 Pare. Di harapkan konselor dapat mengunakan teknik permainan dialog dalam konseling kelompok Gestalt sebagai salah satu alternatif dalam mengurangi keterisolasian siswa yang tinggi. Kata Kunci: Teknik Permainan Dialog, Keterisolasia

The Amazing Old Nova Q Cygni: A Far Ultraviolet Synthetic Spectral Analysis

Q Cygni (Nova Cygni 1876) is the third oldest old novae (after WY Sge and V841 Oph) with a long orbital period of 10.08 hours and spectroscopic peculiarities in the optical including the presence of variable wind outflow revealed by optical P Cygni profiles in the HeI lines and H alpha beta (Kafka et al. 2003). We have carried out a synthetic spectral analysis of a far ultraviolet IUE archival spectrum of Q Cygni using our optically thick, steady state, accretion disk models and model white dwarf photospheres. We find that the accretion light of a luminous accretion disk dominates the FUV flux of the hot component with a rate of accretion 2-3 1.E-9 Msun/yr. We find that Q Cygni lies at a distance of 741 \pm 110 pc . The implications of our results for theoretical predictions for old novae are presented.Comment: PASP, August 201

HST/STIS spectroscopy of the exposed white dwarf in the short-period dwarf nova EK TrA

We present high resolution Hubble Space Telescope ultraviolet spectroscopy of the dwarf nova EK TrA obtained in deep quiescence. The Space Telescope Imaging Spectrograph data reveal the broad Ly-alpha absorption profile typical of a moderately cool white dwarf, overlayed by numerous broad emission lines of He, C, N, and Si and by a number of narrow absorption lines, mainly of CI and SiII. Assuming a white dwarf mass in the range 0.3-1.4Msun we derive Teff=17500-23400K for the primary in EK TrA; Teff=18800K for a canonical mass of 0.6Msun. From the narrow photospheric absorption lines, we measure the white dwarf rotational velocity, v*sin i=200+-100kms. Even though the strong contamination of the photospheric white dwarf absorption spectrum by the emission lines prevents a detailed quantitative analysis of the chemical abundances of the atmosphere, the available data suggest slightly sub-solar abundances. The high time resolution of the STIS data allows us to associate the observed ultraviolet flickering with the emission lines, possibly originating in a hot optically thin corona above the cold accretion disk.Comment: 6 pages A&A-Latex, 5 Figures, accepted for publication in A&

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. II.The optically thin phase and the structure of the ejecta in recurrent novae

We continue our study of the physical properties of the recurrent nova T Pyx, focussing on the structure of the ejecta in the nebular stage of expansion during the 2011 outburst. The nova was observed contemporaneously with the Nordic Optical Telescope (NOT), at high resolution spectroscopic resolution (R ~ 65000) on 2011 Oct. 11 and 2012 Apr. 8 (without absolute flux calibration), and with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope, at high resolution (R ~ 30000) on 2011 Oct. 10 and 2012 Mar. 28 (absolute fluxes). We use standard plasma diagnostics (e.g. [O III] and [N II] line ratios and the H$\beta$ line fluxes) to constrain electron densities and temperatures. Using Monte Carlo modeling of the ejecta, we derive the structure and filling factor from comparisons to the optical and ultraviolet line profiles. The ejecta can be modeled using an axisymmetric conical -- bipolar -- geometry with a low inclination of the axis to the line of sight, i=15+/-5 degrees, compatible with published results from high angular resolution optical spectro-interferometry. The structure is similar to that observed in the other short orbital period recurrent novae during their nebular stages. We show that the electron density scales as $t^{-3}$ as expected from a ballistically ejected constant mass shell; there is no need to invoke a continuing mass outflow following the eruption. The derived mass for the ejecta with filling factor f ~ 3%, M_ej ~ 2E-6$M_sun is similar to that obtained for other recurrent nova ejecta but inconsistent with the previously reported extended optically thick epoch of the explosion. We suggest that the system underwent a common envelope phase following the explosion that produced the recombination event. Implications for the dynamics of the recurrent novae are discussed. (truncated)Comment: accepted for publication in A&A (10 Nov. 2012), 10 pgs, 16 fig

An Illustration of Modeling Cataclysmic Variables: HST, FUSE, SDSS Spectra of SDSSJ080908.39+381406.2

We use FUSE, HST, and SDSS spectra of the cataclysmic variable SDSSJ0809 to illustrate procedures for calculating and testing system models. Our final model has an accretion disk temperature profile similar to the SW Sextantis profile determined from tomographic reconstruction.Comment: 51 pages, 19 Postscript figures, 6 table

ST/STIS Spectroscopy of the White Dwarfs in the Short-Period Dwarf Novae LL And and EF Peg

We present new HST/STIS observations of the short-period dwarf novae LL And and EF Peg during deep quiescence. We fit stellar models to the UV spectra and use optical and IR observations to determine the physical parameters of the whitedwarfs in the systems, the distances to the binaries, and the properties of thesecondary stars. Both white dwarfs are relatively cool, having T_{eff} near 15000K, and consistent with a mass of 0.6 M-sun. The white dwarf in LL And appears to be of solar abundance or slightly lower while that in EF Peg is near 0.1-0.3 solar. LL And is found to be 760 pc away while EF Peg is closer at 380 pc. EF Peg appears to have an ~M5V secondary star, consistent with that expected for its orbital period, while the secondary object in LL And remains a mystery.Comment: Accepted in Ap

Hubble space telescope STIS spectroscopy of the peculiar nova-like variables BK Lyn, V751 Cygni, and V380 Oph

We obtained Hubble STIS spectra of three nova-like variables: V751 Cygni, V380 Oph, and—the only confirmed nova-like variable known to be below the period gap—BK Lyn. In all three systems, the spectra were taken during high optical brightness state, and a luminous accretion disk dominates their far-ultraviolet (FUV) light. We assessed a lower limit of the distances by applying the infrared photometric method of Knigge. Within the limitations imposed by the poorly known system parameters (such as the inclination, white dwarf mass, and the applicability of steady state accretion disks) we obtained satisfactory fits to BK Lyn using optically thick accretion disk models with an accretion rate of for a white dwarf mass of Mwd = 1.2M and for Mwd = 0.4M. However, for the VY Scl-type nova-like variable V751 Cygni and for the SW Sex star V380 Oph, we are unable to obtain satisfactory synthetic spectral fits to the high state FUV spectra using optically thick steady state accretion disk models. The lack of FUV spectra information down to the Lyman limit hinders the extraction of information about the accreting white dwarf during the high states of these nova-like systems

Analisis Pengembangan Pendidikan Wilayah Kepulauan Berbasis Transportasi Laut

Faktor sosial dan fisik-geografis kepulauan menjadi masalah dalam pemerataan proses pendidikan sehingga penyediaan infrastruktur pendidikan pada pulau menjadi penting. Pendekatan metode pendidikan dan alternatif pengembangan infrastruktur dapat dilakukan dengan memanfaatkan moda transportasi laut, yaitu dengan sekolah terapung dan perahu sekolah. Hasil analisis dengan mengembangkan model skenario operasi ketika kondisi peserta konstan atau meningkat menunjukkan konsep pembangunan sekolah di darat untuk setiap wilayah membutuhkan pembiayaan terkecil yaitu Rp 4.137.190.200 atau 18,04% dengan jam pengajaran 288 jam atau 30,34% dan unit biaya Rp 17.888/pax.jam. Akan tetapi, selama periode operasi lima tahun dengan peserta menurun menunjukkan konsep pengembangan perahu sekolah dengan pembiayaan terkecil yaitu Rp 3.672/pax.jam atau 19,05% dengan jam pengajaran 225 jam atau 23,69%. Faktor jarak antar pulau dan spesifikasi teknis armada sangat berpengaruh terhadap opsi pengembangan yang dipilih. Pada penelitian ini, perahu sekolah dipilih jika jarak kurang dari 10 mile. Sedangkan, konsep sekolah terapung dipilih jika jarak wilayah operasi antara 10-40 mile. Jarak wilayah lebih dari 40 mile diperlukan depot khusus karena ratio waktu operasi lebih kecil dari waktu tempuh. Konsep pembiayaan pendidikan kepulauan yang menggunakan moda laut dapat dilakukan dengan pembagian biaya sesuai anggaran pemerintah. Secara investasi didukung dari pihak pemerintah pusat atau daerah karena anggaran yang besar. Sedangkan untuk biaya operasional bisa dilakukan oleh pemerinah kabupaten/kota karena merupakan pelaksana sekolah