The Penn State - Toruń Centre for Astronomy Planet Search stars

Deka-Szymankiewicz, B.; Niedzielski, A.; Adamczyk, M.; Adamów, M.; Nowak, G.; Wolszczan, A.

doi:10.1051/0004-6361/201731696

Cited by 26 publications

(19 citation statements)

References 84 publications

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“…The sample presented in this paper comprises a total of 15 Li-rich giants from PTPS with the highest Li content, A(Li) NLTE ≥ 1.4 (Adamów et al 2014). HD 181368 was added to this list because this star was identified as a giant by Deka-Szymankiewicz et al (2018), and it was found to be a Li-rich giant as well. Twelve objects are the subject of detailed analysis, as new epochs of precise RV were collected in a quest for possible companions around them within the TAPAS project.…”

Section: Sample and Observationsmentioning

confidence: 99%

“…A detailed description of the atmospheric parameters can be found in Zieliński et al (2012) and Niedzielski et al (2016a). Masses, radii, and stellar ages were adopted from Deka-Szymankiewicz et al (2018).…”

Section: Sample and Observationsmentioning

confidence: 99%

“…In addition to TYC 0405-01700-1 and TYC 3314-01371-1 presented in Adamów et al (2014) we found one more Li-rich giant with a stellar companion. HD 181368, originally classified as a subgiant in PTPS sample Niedzielski & Wolszczan (2008), was found by Deka-Szymankiewicz et al (2018) to be actually a giant.…”

Section: Li-rich Giants With Stellar Companionsmentioning

confidence: 99%

“…The source HD 238914 (BD+59 1909, TYC 3917-01107-1) is a V = 8.79 ± 0.01 (Høg et al 2000), π = 1.70 ± 0.23 (Gaia Collaboration 2016) star in Draco. Atmospheric parameters derived by Zieliński et al (2012) are presented in Table 1 together with physical parameters derived by Deka-Szymankiewicz et al (2018). This star is a giant (log g = 2.37) with a mass of M/M = 1.47, radius R/R = 12.73 (Adamczyk et al 2016) and [Fe/H] = −0.25.…”

Section: Hd 238914: a Giant Planet In 57 Au Orbitmentioning

confidence: 99%

“…The source TYC 3318-01333-1 (Gaia 439327806662223744, 2MASS J03021978+4944389) is a V = 9.90 ± 0.03 (Høg et al 2000) and π = 1.80 ± 0.39 (Gaia Collaboration 2016) giant star with T eff = 4776 K, log g = 2.97, and solar metallicity ([Fe/H] = −0.06) in Perseus. According to Deka-Szymankiewicz et al (2018), it has a mass of M/M = 1.19 and a radius of R/R = 5.90. With 12 C/ 13 C = 15 and A(Li) = 1.51, this star was classified as a Li-rich giant after the FDU stage.…”

Section: Tyc 3318-01333-1: a Planet In A Binary Systemmentioning

confidence: 99%

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Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Adamów

Niedzielski

Kowalik

et al. 2018

A&A

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Context. We present the latest results of our search for planets with HARPS-N at the 3.6 m Telescopio Nazionale Galileo under the Tracking Advanced Planetary Systems project: an in-depth study of the 15 most Li abundant giants from the PennState – Toruń Planet Search sample. Aims. Our goals are first, to obtain radial velocities of the most Li-rich giants we identified in our sample to search for possible low-mass substellar companions, and second, to perform an extended spectral analysis to define the evolutionary status of these stars. Methods. This work is based on high-resolution spectra obtained with the Hobby-Eberly Telescope and its High Resolution Spectrograph, and with the HARPS-N spectrograph at the Telescopio Nazionale Galileo. Two stars, HD 181368 and HD 188214, were also observed with UVES at the VLT to determine beryllium abundances. Results. We report i) the discovery of two new planetary systems around the Li-rich giant stars: HD 238914 and TYC 3318-01333-1 (a binary system); ii) reveal a binary Li-rich giant, HD 181368; iii) although our current phase coverage is not complete, we suggest the presence of planetary mass companions around TYC 3663-01966-1 and TYC 3105-00152-1; iv) we confirm the previous result for BD+48 740 and present updated orbital parameters, and v) we find a lack of a relation between the Li enhancement and the Be abundance for the stars HD 181368 and HD 188214, for which we acquired blue spectra. Conclusions. We found seven stars with stellar or potential planetary companions among the 15 Li-rich giant stars. The binary star frequency of the Li-rich giants in our sample appears to be normal, but the planet frequency is twice that of the general sample, which suggests a possible connection between hosting a companion and enhanced Li abundance in giant stars. We also found most of the companions orbits to be highly eccentric.

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Section: Sample and Observationsmentioning

confidence: 99%

Section: Sample and Observationsmentioning

confidence: 99%

Section: Li-rich Giants With Stellar Companionsmentioning

confidence: 99%

Section: Hd 238914: a Giant Planet In 57 Au Orbitmentioning

confidence: 99%

Section: Tyc 3318-01333-1: a Planet In A Binary Systemmentioning

confidence: 99%

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Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Adamów

Niedzielski

Kowalik

et al. 2018

A&A

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On the chemical composition of the evolved very bright metal‐poor star HD 1936

Çalışkan,

Alazzawi,

Nasolo

2024

Astron Nachr

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We present chemical abundances of the very bright metal‐poor star HD 1936 based on high‐resolution and high SNR spectra from AUKR. We obtain the abundances of 29 atomic species with atomic numbers between 3 and 63. In this context, the derived lithium abundance of 1.01 is consistent with the thin Li plateau observed in lower red giant branch stars. The star is a carbon‐normal with a ratio of −0.31, just like other low‐luminosity red giants on the thin Li plateau. We find the ratios of [Eu/Fe] = 0.43 and [Ba/Eu] = −0.64, indicating very little s‐process contamination. These ratios allow us to classify the star as a moderately r‐process‐enhanced (r‐I) metal‐poor star for the first time. It is worth mentioning that the star has a metallicity of −1.74, a [Cu/Fe] of −0.74, a [Zn/Fe] of 0.04, and a [Mg/C] of 0.69. The results suggest that it may be a second‐generation star formed in a multi‐enriched environment, rather than being a descendant of very massive first‐generation stars. A last point worth mentioning is the possibility that HD 1936 may host a sub‐stellar component with a mass of . Although our study does not confirm or deny this, we briefly discuss the possibility of the star hosting a planet.

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A surprise in the updated list of stellar perturbers of long-period comet motion

Wysoczańska

Dybczyński

Polińska

2020

A&A

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Context. The second Gaia data release (Gaia DR2) provided us with the precise five-parameter astrometry for 1.3 billion of sources. As stars passing close to the Solar System are thought to influence the dynamical history of long-period comets, we update and extend the list of stars that could potentially perturb the motion of these comets. Aims. We announce a publicly available database containing an up-to-date list of stars and stellar systems potentially perturbing the motion of long-period comets. We add new objects and revise previously published lists. Special emphasis is placed on stellar systems. A discussion of mass estimation is included. Methods. Using the astrometry, preferably from Gaia DR2, augmented with data from other sources, we calculate nominal spatial positions and velocities for each star. To filter studied objects on the basis of their nominal minimum heliocentric distances we numerically integrate the motion of stars under the Galactic potential and their mutual interactions. Results. We announce the updated list of stellar perturbers of cometary motion, including the masses of perturbers along with the publicly available database interface. These data are ready to be used with the observed long-period comets orbits to study an individual influence of a whole sample of perturbers, or specific stars, on a dynamical past or future of a specific comet. New potential perturbers were added; there are 138 more than in the previously published sources. Conclusions. We demonstrate that a new set of prospective perturbers is an important tool in studies of cometary dynamics. The use of our data changes the results of the past and future cometary motion analysis. We point out a puzzling object in our list, star ALS 9243. The Gaia DR2 astrometry suggests a very close encounter of this star with the Sun; however, its astrophysical parameters result in a completely different current distance of ALS 9243 and its high mass.

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The Penn State - Toruń Centre for Astronomy Planet Search stars

Cited by 26 publications

References 84 publications

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

On the chemical composition of the evolved very bright metal‐poor star HD 1936

A surprise in the updated list of stellar perturbers of long-period comet motion

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