Three red giants with substellar-mass companions

We present three giant stars from the ongoing Penn State-Toru\'n Planet Search with the Hobby-Eberly Telescope, which exhibit radial velocity variations that point to a presence of planetary --mass companions around them. BD+49 828 is a $M=1.52 \pm 0.22$ $M_{\odot}$ K0 giant with a $m sini$=$1.6^{+0.4}_{-0.2}$ $M_{J}$ minimum mass companion in $a=4.2^{+0.32}_{-0.2}$ AU ($2590^{+300}_{-180}$d), $e=0.35^{+0.24}_{-0.10}$ orbit. HD 95127, a log$L$/$L_{\odot}$=$2.28 \pm 0.38$, $R = 20\pm 9$ $R_{\odot}$, $M=1.20 \pm 0.22$ $M_{\odot}$ K0 giant has a $m sini$=$5.01^{+0.61}_{-0.44}$ $M_{J}$ minimum mass companion in $a=1.28^{+0.01}_{-0.01}$ AU ($482^{+5}_{-5}$d), $e=0.11^{+0.15}_{-0.06}$ orbit. Finally, HD 216536, is a $M=1.36 \pm 0.38$ $M_{\odot}$ K0 giant with a $m sin i=1.47^{+0.20}_{-0.12}$ $M_{J}$ minimum mass companion in $a=0.609^{+0.002}_{-0.002}$ AU ($148.6^{+0.7}_{-0.7}$d), $e=0.38^{+0.12}_{-0.10}$ orbit. Both, HD 95127 b and HD 216536 b in their compact orbits, are very close to the engulfment zone and hence prone to ingestion in the near future. BD+49 828 b is among the longest period planets detected with the radial velocity technique until now and it will remain unaffected by stellar evolution up to a very late stage of its host. We discuss general properties of planetary systems around evolved stars and planet survivability using existing data on exoplanets in more detail.Comment: 47 pages, 11 figures. Accepted by Ap

TAPAS IV. TYC 3667-1280-1 b - the most massive red giant star hosting a warm Jupiter

We present the latest result of the TAPAS project that is devoted to intense monitoring of planetary candidates that are identified within the PennState-Toru\'n planet search. We aim to detect planetary systems around evolved stars to be able to build sound statistics on the frequency and intrinsic nature of these systems, and to deliver in-depth studies of selected planetary systems with evidence of star-planet interaction processes. The paper is based on precise radial velocity measurements: 13 epochs collected over 1920 days with the Hobby-Eberly Telescope and its High-Resolution Spectrograph, and 22 epochs of ultra-precise HARPS-N data collected over 961 days. We present a warm-Jupiter ($T_{eq}=1350 K$, $m_{2} sin i=5.4\pm$0.4$M_{J}$) companion with an orbital period of 26.468 days in a circular ($e=0.036$) orbit around a giant evolved ($\log g=3.11\pm0.09$, $R=6.26\pm0.86R_{\odot}$) star with $M_{\star}=1.87\pm0.17M_{\odot}$. This is the most massive and oldest star found to be hosting a close-in giant planet. Its proximity to its host ($a=0.21au$) means that the planet has a $13.9\pm2.0\%$ probability of transits; this calls for photometric follow-up study. This massive warm Jupiter with a near circular orbit around an evolved massive star can help set constraints on general migration mechanisms for warm Jupiters and, given its high equilibrium temperature, can help test energy deposition models in hot Jupiters.Comment: 5 pages, 3 figures, accepted by A&

TAPAS - Tracking Advanced Planetary Systems with HARPS-N. II. Super Li-rich giant HD 107028

Lithium rich giant stars are rare objects. For some of them, Li enrichment exceeds abundance of this element found in solar system meteorites, suggesting that these stars have gone through a Li enhancement process. We identified a Li rich giant HD 107028 with A(Li) > 3.3 in a sample of evolved stars observed within the PennState Torun Planet Search. In this work we study different enhancement scenarios and we try to identify the one responsible for Li enrichment for HD 107028. We collected high resolution spectra with three different instruments, covering different spectral ranges. We determine stellar parameters and abundances of selected elements with both equivalent width measurements and analysis, and spectral synthesis. We also collected multi epoch high precision radial velocities in an attempt to detect a companion. Collected data show that HD 107028 is a star at the base of Red Giant Branch. Except for high Li abundance, we have not identified any other anomalies in its chemical composition, and there is no indication of a low mass or stellar companion. We exclude Li production at the Luminosity Function Bump on RGB, as the effective temperature and luminosity suggest that the evolutionary state is much earlier than RGB Bump. We also cannot confirm the Li enhancement by contamination, as we do not observe any anomalies that are associated with this scenario. After evaluating various scenarios of Li enhancement we conclude that the Li-overabundance of HD 107028 originates from Main Sequence evolution, and may be caused by diffusion process.Comment: Accepted for publication in A&

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N. V.: A Massive Jupiter orbiting the very low metallicity giant star BD+03 2562 and a possible planet around HD~103485

We present two evolved stars from the TAPAS (Tracking Advanced PlAnetary Systems) with HARPS-N project devoted to RV precision measurements of identified candidates within the PennState - Torun Centre for Astronomy Planet Search. Evolved stars with planets are crucial to understand the dependency of the planet formation mechanism on the mass and metallicity of the parent star and to study star-planet interactions. The paper is based on precise radial velocity (RV) measurements, for HD 103485 we collected 57 epochs over 3317 days with the Hobby-Eberly Telescope and its High Resolution Spectrograph and 18 ultra-precise HARPS-N data over 919 days. For BD+03 2562 we collected 46 epochs of HET data over 3380 days and 19 epochs of HARPS-N data over 919 days. We present the analysis of the data and the search for correlations between the RV signal and stellar activity, stellar rotation and photometric variability. Based on the available data, we interpret the RV variations measured in both stars as Keplerian motion. Both stars have masses close to Solar (1.11 and 1.14), very low metallicities ([Fe/H]=-0.50 and -0.71), and, both have Jupiter planetary mass companions (m sin i=7 and 6.4 Mj), in close to terrestrial orbits (1.4 and 1.3~au), with moderate eccentricities (e=0.34 and 0.2). However, we cannot totally exclude that the signal in the case of HD~103485 is due to rotational modulation of active regions. Based on the current data, we conclude that BD+03 2562 has a bona fide planetary companion while for HD 103485 we cannot totally exclude that the best explanation for the RV signal modulations is not the existence of a planet but stellar activity. If, the interpretation remains that both stars have planetary companions they represent systems orbiting very evolved stars with very low metallicities, a challenge to the conditions required for the formation of massive giant gas planets.Comment: Acepted A&A 12 pages, 11 figure

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N. III. HD 5583 and BD+15 2375 - two cool giants with warm companions

Evolved stars are crucial pieces to understand the dependency of the planet formation mechanism on the stellar mass and to explore deeper the mechanism involved in star-planet interactions. Over the past ten years, we have monitored about 1000 evolved stars for radial velocity variations in search for low-mass companions under the Penn State - Torun Centre for Astronomy Planet Search program with the Hobby-Eberly Telescope. Selected prospective candidates that required higher RV precision measurements have been followed with HARPS-N at the 3.6 m Telescopio Nazionale Galileo under the TAPAS project. We aim to detect planetary systems around evolved stars to be able to build sound statistics on the frequency and intrinsic nature of these systems, and to deliver in-depth studies of selected planetary systems with evidence of star-planet interaction processes. For HD 5583 we obtained 14 epochs of precise RV measurements collected over 2313 days with the Hobby-Eberly Telescope (HET), and 22 epochs of ultra-precise HARPS-N data collected over 976 days. For BD+15 2375 we collected 24 epochs of HET data over 3286 days and 25 epochs of HARPS-S data over 902 days. We report the discovery of two planetary mass objects orbiting two evolved Red Giant stars: HD~5583 has a m sin i = 5.78 M$_{J}$ companion at 0.529~AU in a nearly circular orbit (e=0.076), the closest companion to a giant star detected with the RV technique, and BD+15~2735 that with a m sin i= 1.06 M$_{J}$ holds the record of the lightest planet found so far orbiting an evolved star (in a circular e=0.001, 0.576~AU orbit). These are the third and fourth planets found within the TAPAS project, a HARPS-N monitoring of evolved planetary systems identified with the Hobby-Eberly Telescope.Comment: 9 pages, 6 figures. Accepted by Astronomy and Astrophysic

Wplyw ledzwianu siewnego jako rosliny regenerujacej na plonowanie roslin w plodozmianie na glebie lekkiej

Eksperyment polowy przeprowadzono w Gospodarstwie Doświadczalnym Uhrusk, należącym do AR w Lublinie. Obiektem badań było żyto ozime (roślina testowa) i pozostałe rośliny uprawiane w trzech płodozmianach i monokulturze zbożowej na tle dwóch poziomów agrotechniki. Szczególną uwagę poświęcono oddziaływaniu przedplonu i przedprzedplonu na plonowanie i zachwaszczenie rośliny testowej (żyta ozimego) oraz roślin wchodzących w skład badanych zmianowań. Żyto ozime najwyżej plonowało w płodozmianie z udziałem lędźwianu siewnego, a plon ziarna wynosił 3,9 t z ha. W pozostałych płodozmianach obniżka plonu wynosiła od 4,1% do 5,6%, zaś w monokulturze 12,8%. Nastąpiło również pogorszenie struktury plonu żyta ozimego (masa tysiąca zieren - MTZ i masa ziarna z kłosa i rośliny) uprawianego w zmianowaniach bez udziału lędźwianu siewnego. Wyższy poziom agrotechniki korzystnie wpłynął na plonowanie żyta ozimego i pozostałych roślin w badanych płodozmianach i monokulturze. Stopień zachwaszczenia żyta ozimego był ściśle związany z płodozmianem, w którym wysiewano żyto, i był on najniższy w zmianowaniu z udziałem lędźwianu siewnego. W pozostałych zmianowaniach zachwaszczenie wyrażone liczbą i biomasą chwastów wzrosło odpowiednio o 26,5% i 32,8%, zaś w monokulturze 65,2% i 93,9%.Field experiment was carried out in Uhrusk Experimental Farm, a part of Agricultural University in Lublin. The research object was winter rye (test plant) and the other plants cultivated in three crop rotations and in cereal monoculture against two agrotechnical levels. Special concern was given to the influence of forecrop and foreforecrop on yielding and weed infestation of test plant (winter rye) as well as the other plants included into studied crop rotations. Winter rye reached the highest yielding in the crop rotation with chickling vetch at grain yield 3.9 t·ha⁻¹. In other crop rotations the yield decrease ranged from 4.1% to 5.6%, whereas as high as 12.8% in monoculture. Deterioration of yielding structure occured in winter rye (mass of 1000 grains, and weight of grains per ear and plant) in rotations without chickling vetch. A higher agrotechnics level affected favourably the yielding of winter rye and other plants in examined crop rotations and in monoculture. Weed infestation degree of winter rye was closely linked with crop rotation where the rye was sown and it was the lowest in crop rotation with chickling vetch. Weed infestation in other crop rotations expressed by weed number and biomass increased by 26.5% and 32.8% respectively, while in the monoculture - by 65.2% and 93.9%

Yield-forming effect of the crop rotation without farmyard manure under sandy soil conditions

Целью точного полевого опыта было сравнение продуктивности двух севооборотов, без стойлового навоза и со стойловым навозом,при трех уровнях удобрения NPK под картофель. В безнавозном севообороте органическим удобрением являлись сидеральные удобрения. В опытах установлено различное реагирование отдельных видов растений, выраженное урожаями, на вид органического удобрения в севооборотах. Картофель как тестовая культура для органического удобрения характеризовался высшими урожаями на стойловом навозе, чем на сидеральных удобрениях. Наиболее благоприятной для картофеля в уело виях песчаных почв Угруска оказалась, независимо от вида органического удобрения, лозв 315 кг HPK на гектар. В общем можно констетиро вать, что в первой севооборотной ротации периода 1977-1980.гг. образующий урожай эффект безнавозного севооборота незначительно откло няется на плюс от общей продуктивности севооборота со стойловым навозом.The aim of the respective exact field experiment was to compare the productivity of two crop rotations: without and with farmyard manure at 3 NPK fertilization levels for potatoes. In the crop rotation without farmyard manure organic fertilization constituted green manure. Different response of particular crops expressed in terms of yield magnitude to the organic fertilization in crop rotations has been found in theexperiment. Potatoes as a crop testing the organic fertilization distinguished itself with higher yields on farmyard than on green manure. The most favourable for potatoes under conditions of sandy soil in the Uhrusk region proved to be the rate of 315 kg NPK per hectare. On the whole, it could be stated that in the first crop rotation of 1977-1980 the yield-forming effect of the crop rotation without farmyard manure deviated only slightly in plus from global productivity of the crop rotation with farmyard manure