Abstract
WASP-43 b is one of the most important candidates for detecting an orbital decay. We investigate pieces of evidence for this expectation as variations in its transit timings, based on the ...ground and space observations. The data set includes the transit observations at the TÜBİTAK National Observatory of Turkey and Transiting Exoplanet Survey Satellite (TESS). We present a global model of the system, based on the most precise photometry from space, ground, and archival radial velocity data. Using the homogenized data set and modeled light curves, we measure the mid-transit times for WASP-43 b. Our analysis agrees with a linear ephemeris for which we refine the light elements for future observations of the system. However, there is a negative difference between the transit timings derived from TESS data in two sectors (9 and 35) and a hint of an orbital period decrease in the entire data set. Both findings are statistically insignificant due to the short baseline of observations, which prevents us from drawing firm conclusions about the orbital decay of this ultra-short-period planet. However, assuming the effect of this decrease of the period in the planet's orbit, we derive a lower limit for the reduced tidal quality factor as
Q
*
′
>
(
4.01
±
1.15
)
×
10
5
from the best-fitting quadratic function. Finally, we calculate a probable rotational period for this system as 7.52 days from the out-of-transit flux variation in the TESS light curves due to spot modulation.
Some of the most scientifically valuable transiting planets are those that were already known from radial velocity (RV) surveys. This is primarily because their orbits are well characterized and they ...preferentially orbit bright stars that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite (TESS) provides an opportunity to survey most of the known exoplanet systems in a systematic fashion to detect possible transits of their planets. HD 136352 (Nu2 Lupi) is a naked-eye (V = 5.78) G-type main-sequence star that was discovered to host three planets with orbital periods of 11.6, 27.6, and 108.1 days via RV monitoring with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph. We present the detection and characterization of transits for the two inner planets of the HD 136352 system, revealing radii of R⊕ and R⊕ for planets b and c, respectively. We combine new HARPS observations with RV data from the Keck/High Resolution Echelle Spectrometer and the Anglo-Australian Telescope, along with TESS photometry from Sector 12, to perform a complete analysis of the system parameters. The combined data analysis results in extracted bulk density values of g cm−3 and g cm−3 for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multitransiting planet system, the bright host star, and the diversity of planetary interiors and atmospheres means this will likely become a cornerstone system for atmospheric and orbital characterization of small worlds.
Prevalence of bone and soft tissue tumors Yücetürk, Güven; Sabah, Dündar; Keçeci, Burçin ...
Acta orthopaedica et traumatologica Turcica/Acta orthopaedica et traumatologica turcica,
2011, Letnik:
45, Številka:
3
Journal Article
Recenzirano
Odprti dostop
Multidisciplinary approach is a necessity for the appropriate diagnosis and treatment of bone and soft tissue tumors. The Ege University Musculoskeletal Tumor Council offers consultation services to ...other hospitals in the Aegean region. Since 1988 the Council has met weekly and spent approximately 1,500 hours evaluating almost 6,000 patients with suspected skeletal system tumors. Our objective was to present the data obtained from this patient group.
A total of 5,658 patients, suspected to have a musculoskeletal tumor, were evaluated retrospectively. Multiple records of the patients due to multiple attendance to the Council were excluded. The prevalance of the bone and soft tissue tumors in these patients were analysed.
Malignant mesenchymal tumors accounted for 39.7% of the total patients, benign tumors for 17%, tumor-like lesions for 17.8% and metastatic carsinomas for 8.6%. Malignant bone tumors were 50.2% and malignant soft tissue tumors were 49.8% of all the sarcomas. Among the malignant bone tumors the most common was osteosarcomas at a rate of 33.6%, followed by Ewing-PNET at 25.5%, chondrosarcomas at 19.4% and haematopoietic tumors at 17.6%. Pleomorphic sarcomas (24.5%), liposarcoma (16.4%), synovial sarcoma (13%) and undifferential sarcomas (8.8%) were the most common types of malignant sof tissue tumors. Benign soft tissue tumors (48%), benign cartilage tumors (28%), giant cell tumor (15%) and osteogenic tumors (9%) were found among the benign tumors. Hemangioma, lipoma, agressive fibromatosis, enchondroma, solitary chondroma and osteoid osteoma were the most common tumors in their groups. Lung (27%), breast (24%), gastrointestinal system (10.5%) and kidney (8.2%) carcinomas were the most common primary sites of the bone metastasis.
Turkey still lacks a comprehensive series indicating the incidence and diagnostic distribution of bone and soft tissue tumors. The presented data would add to our knowledge on the specific rates of the bone and soft tissue tumors in Aegean region.
WASP-43 b is one of the most important candidates for detecting an orbital decay. We investigate pieces of evidence for this expectation as variations in its transit timings, based on the ground and ...space observations. The data set includes the transit observations at the TUBITAK National Observatory of Turkey and Transiting Exoplanet Survey Satellite (TESS). We present a global model of the system, based on the most precise photometry from space, ground, and archival radial velocity data. Using the homogenized data set and modeled light curves, we measure the mid-transit times for WASP-43 b. Our analysis agrees with a linear ephemeris for which we refine the light elements for future observations of the system. However, there is a negative difference between the transit timings derived from TESS data in two sectors (9 and 35) and a hint of an orbital period decrease in the entire data set. Both findings are statistically insignificant due to the short baseline of observations, which prevents us from drawing firm conclusions about the orbital decay of this ultra-short-period planet. However, assuming the effect of this decrease of the period in the planet's orbit, we derive a lower limit for the reduced tidal quality factor as Q'_* > (4.01 +_ 1.15). 10^5 from the best-fitting quadratic function. Finally, we calculate a probable rotational period for this system as 7.52 days from the out-of-transit flux variation in the TESS light curves due to spot modulation.
Doğu Anadolu Gözlemevi'nde (DAG) kurulmakta olan 4 metrelik teleskop, kızılöte dalgaboylarında yapabileceği gezegen örtülme gözlemleri ile ötegezegen atmosferlerini anlamaya yönelik çalışmalara ...önemli katkı yapabilecek potansiyele sahiptir. Bu potansiyele yönelik bir ön-değerlendirme yapabilmek amacıyla bu çalışmada öncelikle geçiş yapan ötegezegenlerin gece-gündüz arası ısı transferinin mükemmel olduğu ve yakın kızılötede yansıtma güçlerinin sıfır olduğu varsayımlarıyla denge sıcaklıkları hesaplanmıştır. Ayrıca, denge sıcaklıklarında birer karacisim olduğu varsayılan geçiş yapan ötegezegenlerin J, H ve K bantlarında örtülme derinlikleri hesaplanmıştır. {\sc{signal}} kodu ile 4 metre sınıfında bir teleskop ve DAG'da kurulmakta olan 4 metrelik teleskobun kızılöte kamerasına benzer özelliklere sahip bir dedektör ile 6 - 15.5 kadir aralığında 0.5 kadirlik adımlarla J, H ve K bandında ulaşılabilecek Sinyal / Gürültü değerleri hesaplanmıştır. Bu değerler örtülme derinlikleri ile karşılaştırılarak birçok sıcak-Jüpiter türü gezegenin örtülmelerinin gözlenmesi için yeterli fotometrik hassasiyete ulaşılabileceği sonucuna varılmıştır. Ayrıca kızılöte dedektörün gökyüzünde gördüğü alanın küçük olması sebebiyle oluşabilecek kırmızı gürültü kaynaklarının neler olabileceği tartışılmıştır. Hedef ve mukayese yıldızın peş peşe gözlenerek diferansiyel fotometri tekniği ile bu gürültünün azaltılabileceği ve yüksek hassasiyetli geçiş gözlemlerinden elde edilebilecek bilgilerin Gaussyen Süreçler tekniğinde kullanılarak geriye kalan kırmızı gürültünün modellenebileceği önerilmiştir.
We present the potential of currently installing 4 meter telescope of DAG for the exoplanet atmosphere studies with the occultation observations. In order, equilibrium temperatures ($T_{eq}$) of transiting exoplanets are calculated assuming perfect heat redistribution between the day and night sides and no reflection. Using $T_{eq}$ values, occultation depths in the near-infrared J, H and K bands are calculated with the assumption that the host star and the exoplanets were blackbodies. Then, the hypothetical Signal-to-Noise ratios are calculated for the J, H, and K bands employing the {\sc signal} code for a 4 meter class telescope with a similar infrared camera to that planned to be used with the 4 meter telescope Doğu Anadolu Gözlemevi. The calculations are performed in the 6 - 15.5 magnitude range for each band with 0.5 magnitude steps. We compare the signal-to-noise ratio values with the hypothetical occultation depths and conclude that photometric precision requirements for accultation observations can be satisfied for many hot-Jupiters especially in the K band. We discuss the potential sources of correlated noise due to the small field of view provided by the infrared camera and suggest that the simultaneous observations of the target and comparison star can mitigate the correlated noise, the remains of which can be modelled by employing Gaussian Processes and then removed with the prior knowledge from high precision transit observations.
The binary star NY Hya is a bright, detached, double-lined eclipsing system with an orbital period of just under five days with two components each nearly identical to the Sun and located in the ...solar neighbourhood. The objective of this study is to test and confront various stellar evolution models for solar-type stars based on accurate measurements of stellar mass and radius. We present new ground-based spectroscopic and photometric as well as high-precision space-based photometric and astrometric data from which we derive orbital as well as physical properties of the components via the method of least-squares minimisation based on a standard binary model valid for two detached components. Classic statistical techniques were invoked to test the significance of model parameters. Additional empirical evidence was compiled from the public domain; the derived system properties were compared with archival broad-band photometry data enabling a measurement of the system's spectral energy distribution that allowed an independent estimate of stellar properties. We also utilised semi-empirical calibration methods to derive atmospheric properties from Str\"{o}mgren photometry and related colour indices. Data was used to confront the observed physical properties with classic and magnetic stellar evolution models.
We study the most precise light curves of the planet-host HAT-P-36 that we obtained from the ground primarily with a brand-new 80 cm telescope very recently installed at Ankara University Kreiken ...Observatory of Turkey and also from the space with Transiting Exoplanet Survey Satellite. The main objective of the study is to analyze the Transit Timing Variations (TTV) observed in the hot-Jupiter type planet HAT-P-36 b, a strong candidate for orbital decay, based on our own observations as well as that have been acquired by professional and amateur observers since its discovery. HAT-P-36 displays out-of-transit variability as well as light curve anomalies during the transits of its planet due to stellar spots. We collected and detrended all the complete transit light curves we had access to from these anomalies, which we modeled with EXOFAST and measured the mid-transit times forming a homogeneous data set for a TTV analysis. We found an increase in the orbital period of HAT-P-36 b at a rate of 0.014 s per year from the best fitting quadratic function, which is only found in the TTV constructed by making use of the mid-transit times measured from detrended light curves, against an expectation of an orbital decay based on its parameters. We refined the values of these system parameters by modeling the Spectral Energy Distribution of the host star, its archival radial velocity observations from multiple instruments, and most precise transit light curves from the space and the ground covering a wide range of wavelengths with EXOFASTV2. We also analyzed the out-of-transit variability from TESS observations to search for potential rotational modulations through a frequency analysis. We report a statistically significant periodicity in the TESS light curve at 4.22 +/- 0.02 d, which might have been caused by instrumental systematics but should be tracked in the future observations of the target.
Some of the most scientifically valuable transiting planets are those that were already known from radial velocity (RV) surveys. This is primarily because their orbits are well characterized and they ...preferentially orbit bright stars that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite ({\it TESS}) provides an opportunity to survey most of the known exoplanet systems in a systematic fashion to detect possible transits of their planets. HD~136352 (Nu\(^2\)~Lupi) is a naked-eye (\(V = 5.78\)) G-type main-sequence star that was discovered to host three planets with orbital periods of 11.6, 27.6, and 108.1 days via RV monitoring with the HARPS spectrograph. We present the detection and characterization of transits for the two inner planets of the HD~136352 system, revealing radii of \(1.482^{+0.058}_{-0.056}\)~\(R_\oplus\) and \(2.608^{+0.078}_{-0.077}\)~\(R_\oplus\) for planets b and c, respectively. We combine new HARPS observations with RV data from Keck/HIRES and the AAT, along with {\it TESS} photometry from Sector 12, to perform a complete analysis of the system parameters. The combined data analysis results in extracted bulk density values of \(\rho_b = 7.8^{+1.2}_{-1.1}\)~gcm\(^{-3}\) and \(\rho_c = 3.50^{+0.41}_{-0.36}\)~gcm\(^{-3}\) for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multi-transiting planet system, the bright host star, and the diversity of planetary interiors and atmospheres means this will likely become a cornerstone system for atmospheric and orbital characterization of small worlds.
We investigate the orbital decay behavior of the well-studied hot Jupiter WASP-12\,b orbiting its late-F host star on a 1.09-day orbit by analyzing its transit timings. Thanks to precise photometric ...data covering nearly 15 years of observations from the space and the ground since the discovery of the planet, including a transit light curve of our own, it became possible to study this behaviour in its details. This work updates the orbital period to a new value of
$P = 1.0914202527 \pm 0.000000039\,\text{days}$ and agrees with the previous finding that the planetary orbit has been shrinking with an updated rate of $-31.03 \pm 0.94\,\text{ms yr}^{-1}$. This corresponds to an orbital decay timescale of $\tau =P/|\dot{P}| = 3.04 \pm 0.09\,\text{Myr}$ that we attribute to the strong tidal interactions between the host-star and the planet. We also update the reduced stellar tidal quality factor as $Q_{*}^{\prime} = (1.72 \pm 0.39) \times$ $10^{5}$, which corresponds to the lower bound of the previously reported values of the parameter.
Bu çalışmada, geç F tayf türünden bir barınak yıldızın etrafında 1.09 günlük bir yörünge döneminde dolanan, çok çalışılmış WASP-12\,b sıcak Jupiter türü gezegenin geçiş zamanlarını inceleyerek yörüngenin küçülme davranışı gösterip göstermediğini araştırdık. Keşfinden beri, neredeyse 15 yılı kapsayan, hem uzaydan hem yerden elde edilen fotometrik veri, hem de bizim kendimize ait bir gözlemimiz sayesinde, bahsi geçen yörünge küçülmesini detaylarıyla incelemek mümkün oldu. Bu çalışma gezegenin yörünge dönemini $P = 1.0914202527 \pm 0.000000039\,\text{gün}$ olarak güncellemesinin yanı sıra gezegenin yörüngesinin sabit bir oran ile küçüldüğünü doğrulamakta ve bu oran $-31.03 \pm 0.94\,\text{ms yıl}^{-1}$ olarak verilmektedir. Bu bulgunun işaret ettiği yörünge küçülmesi zaman ölçeği $\tau=P/|\dot{P}|= 3.04 \pm 0.09\,\text{Milyon yıl}$ olarak bulunmuştur. Yörünge dönemindeki bu kısalma gezegen ve barınak yıldızı arasındaki tedirginlik etkilerine atfedilmiştir. Ek olarak, bu çalışmada yıldızın tedirginlik etkileşmeleri sonucu açığa çıkan enerjiyi alma kapasitesini ifade eden tedirginlik kalite faktörü $Q_{*}^{'} = (1.72 \pm 0.39)\times 10^{5}$ olarak bulunmuştur. Bu değer, daha önceki çalışmalarda rapor edilmiş değer aralığının alt sınırındadır.
Bu çalışmada, Ankara Üniversitesi Bilimsel Araştırma Projeleri (BAP) kapsamında Ankara Üniversitesi Kreiken Rasathanesi’ne kazandırılan Ritchey-Chrétien optik tasarıma ve Nasmyth odak sistemine sahip ...T80 Prof. Dr. Berahitdin Albayrak Teleskobu ile odak düzlemi aletlerinin teknik özellikleri verildi. Gerçekleştirilen test gözlemleri yardımıyla sistemin tayfsal ve fotometrik gözlem performansına yönelik belirlenen parametreler (limit parlaklık, takip ve hizalama hassasiyeti, çözünürlük gibi) ile birlikte yapılan gözlemlerden elde edilen bazı bilimsel sonuçlar sunuldu.
We present the technical specifications of the 80 cm T80 Prof. Dr. Berahitdin Albayrak Telescope of Ankara University Kreiken Observatory and the focal plane instruments installed at its Nasmyth focii, which were all funded by the Ankara University Coordination Office for Scientific Research Projects (BAP) within this contribution. We also provide observational properties, such as brightness limits, tracking and pointing accuracy and precision, spectral and angular resolution, based on the photometric and spectroscopic test observations.
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