A search for star-planet interactions in the υ Andromedae system at X-ray and optical wavelengths

Context. Close-in, giant planets are expected to influence their host stars via tidal or magnetic interaction. But are these effects in X-rays strong enough in suitable targets known so far to be observed with today's instrumentation? Aims: The υ And system, an F8V star with a Hot Jupiter, was observed to undergo cyclic changes in chromospheric activity indicators with its innermost planet's period. We aim to investigate the stellar chromospheric and coronal activity over several months. Methods: We therefore monitored the star in X-rays as well as at optical wavelengths to test coronal and chromospheric activity indicators for planet-induced variability, making use of the Chandra X-ray Observatory as well as the echelle spectrographs FOCES and HRS at Calar Alto (Spain) and the Hobby-Eberly Telescope (Texas, US). Results: The stellar activity level is low, as seen both in X-rays as in Ca ii line fluxes; the chromospheric data show variability with the stellar rotation period. We do not find activity variations in X-rays or in the optical that can be traced back to the planet. Conclusions: Gaining observational evidence of star-planet interactions in X-rays remains challenging.

Star-planet interactions and selection effects from planet detection methods

Planets may have effects on their host stars by tidal or magnetic interaction. Such star-planet interactions are thought to enhance the activity level of the host star. However, stellar activity also affects the sensitivity of planet detection methods. Samples of planet-hosting stars which are investigated for such star-planet interactions are therefore subject to strong selection effects which need to be taken into account.

Hydrogel-forming microneedle arrays made from light-responsive materials for on-demand transdermal drug delivery

We describe, for the first time, stimuli-responsive hydrogel-forming microneedle (MN) arrays that enable delivery of a clinically-relevant model drug (ibuprofen) upon application of light. MN arrays were prepared using a polymer prepared from 2-hydroxyethyl methacrylate (HEMA) and ethylene glycol dimethacrylate (EGDMA) by micromolding. The obtained MN arrays showed good mechanical properties. The system was loaded with up to 5% (w/w) ibuprofen included in a light-responsive 3,5-dimethoxybenzoin conjugate. Raman spectroscopy confirmed the presence of the conjugate inside the polymeric MN matrix. In vitro, this system was able to deliver up to three doses of 50 mg of ibuprofen upon application of an optical trigger over a prolonged period of time (up to 160 hours). This makes the system appealing as a controlled release device for prolonged periods of time. We believe that this technology has potential for use in ?on-demand? delivery of a wide range of drugs in a variety of applications relevant to enhanced patient care.

INVESTIGATING THE ROLE OF NOX NADPH OXIDASE SIGNALLING IN CELL MIGRATION AND ANGIOGENESIS OF ENDOTHELIAL COLONY-FORMING CELLS

Introduction. Endothelial colony-forming cells (ECFCs) hold great cytotherapeutic potential for ischaemic disease. Emerging evidence supports a key role for NADPH oxidases in underlying angiogenic processes of these and other endothelial cells. Aims. To study the influence of Nox NADPH oxidases on the pro-angiogenic function of ECFCs. Methods. Human ECFCs isolated from umbilical cord blood were treated with pro-oxidant PMA and assessed in vitro, both under basal conditions and after siRNA knockdown of Nox4, a key endothelial NADPH oxidase isoform, alongside primary mature human aortic endothelial cells (HAoECs) for comparison, using an established scratch-wound assay as the functional end-point. Results. PMA (500nM for 8h) increased cell migration (control 18.6±2.8, PMA 32.7±6.6% wound closure; n=6, P<0.05) in a superoxide-dependent manner, as indicated by attenuation of this effect in the presence of PEG-SOD. Although HAoEC migration in response to PMA also tended to increase, this did not reach statistical significance. Notably, cell migration at 16h was reduced by Nox4 knockdown in ECFCs (control siRNA 53.4±3.5, Nox4 siRNA 35.1±4.9% closure; n=3, P<0.05), but not in HAoECs, whilst the pro-migratory effect of PMA in ECFCs was potentiated after Nox4 knockdown (control siRNA 53.4±3.5, +PMA 61.5±3.2% closure; n=3, P=NS; Nox4 siRNA 35.1±4.9, +PMA 53.0±4.9% closure; n=3, P<0.05). Conclusion. ECFC migration is enhanced by low concentrations of superoxide, to a greater extent compared to mature endothelial cells, and appears to be at least partly dependent upon NADPH oxidase, including a specific role for Nox4. Although, the precise contribution of endothelial Nox NADPH oxidases isoforms remains to be determined, it is clear that these findings may have significant implications for potential ECFC-based therapies for ischaemic disease, which is associated with an oxidative microenvironment.

EFFECTS OF ENVIRONMENTAL ANTIOXIDANTS ON PRO-ANGIOGENIC ROS SIGNALLING IN ENDOTHELIAL COLONY FORMING CELLS IN VITRO

Introduction. Endothelial colony-forming cells (ECFCs) hold great cytotherapeutic potential for ischaemic disease. Whilst increasing evidence supports a key role for reactive oxygen species (ROS), specifically those derived from Nox NADPH oxidases, in the underlying angiogenic processes of these and other endothelial cells, such studies investigating the role of redox signalling may be hampered by the standard inclusion of antioxidant agents in endothelial cell media, such as phenol red. Aims. To study the effects of antioxidants present in culture media on pro-angiogenic function of ECFCs in vitro. Methods. Human ECFCs isolated from umbilical cord blood were maintained in media with and without antioxidant components (EGM2 and phenol red-free DMEM, respectively) prior to treatment with pro-oxidant PMA and assessment of their in vitro migratory capacity using a scratch-wound assay to measure pro-angiogenic activity. Results. Our previous work in our group indicated that PMA (500nM) increased ECFC migration in a both a superoxide and NADPH oxidase-dependent manner (control 18.6±2.8, PMA 32.7±6.6% wound closure; n=6, P<0.05), as indicated by attenuation with PEG-SOD and VAS2870. However, inconsistencies in the data generated under varying experimental conditions led us to hypothesise that antioxidant agents in the standard ECFC media may be influencing these effects. Indeed, a direct comparison of cell migration between ECFCs incubated in EGM2 DMEM demonstrated a clear trend towards higher migration in the latter (EGM2 9.0±4.5, DMEM 22.7±6.4%; n=3, P=NS). Similar to our previous EGM2 studies, cell migration was potentiated by PMA (control 11.6±1.6, PMA 25.1±2.8%; n=3, P<0.05), but at a lower dose (100nM), which is consistent with a reduction in media antioxidants. Notably, this response was attenuated by VAS2870 (PMA 37.6±7.3, PMA+VAS2870 10.3±2.9%; n=6, P<0.05), underlining a likely role for Nox NADPH oxidases. Conclusion. Taken together, these data indicate that ECFC migration is sensitive to different endothelial cell growth media, which appears to be dependent upon their antioxidant content. Although further experiments, such as quantification of cellular superoxide generation by dihydroethidium fluorescence may be required to confirm a specific role for antioxidants, such blunting of ROS signalling in vitro is clearly an important consideration which may significantly impact upon data interpretation.

Hydrogel-forming microneedle arrays: Potential for use in minimally-invasive lithium monitoring

We describe, for the first time, hydrogel-forming microneedle (MN) arrays for minimally-invasive extraction and quantification of lithium in vitro and in vivo. MN arrays, prepared from aqueous blends of hydrolysed poly(methyl-vinylether-co-maleic anhydride) and crosslinked by poly(ethyleneglycol), imbibed interstitial fluid (ISF) upon skin insertion. Such MN were always removed intact. In vitro, mean detected lithium concentrations showed no significant difference following 30 min MN application to excised neonatal porcine skin for lithium citrate concentrations of 0.9 and 2 mmol/l. However, after 1 h application, the mean lithium concentrations extracted were significantly different, being appropriately concentration-dependent. In vivo, rats were orally dosed with lithium citrate equivalent to 15 mg/kg and 30 mg/kg lithium carbonate, respectively. MN arrays were applied 1 h after dosing and removed 1 h later. The two groups, having received different doses, showed no significant difference between lithium concentrations in serum or MN. However, the higher dosed rats demonstrated a lithium concentration extracted from MN arrays equivalent to a mean increase of 22.5 % compared to rats which received the lower dose. Hydrogel-forming MN clearly have potential as a minimally-invasive tool for lithium monitoring in out-patient settings. We will now focus on correlation of serum and MN lithium concentrations.

The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems

When a planet transits its host star, it blocks regions of the stellar surface from view; this causes a distortion of the spectral lines and a change in the line-of-sight (LOS) velocities, known as the Rossiter-McLaughlin (RM) effect. Since the LOS velocities depend, in part, on the stellar rotation, the RM waveform is sensitive to the star-planet alignment (which provides information on the system’s dynamical history). We present a new RM modelling technique that directly measures the spatially-resolved stellar spectrum behind the planet. This is done by scaling the continuum flux of the (HARPS) spectra by the transit light curve, and then subtracting the infrom the out-of-transit spectra to isolate the starlight behind the planet. This technique does not assume any shape for the intrinsic local profiles. In it, we also allow for differential stellar rotation and centre-to-limb variations in the convective blueshift. We apply this technique to HD 189733 and compare to 3D magnetohydrodynamic (MHD) simulations. We reject rigid body rotation with high confidence (>99% probability), which allows us to determine the occulted stellar latitudes and measure the stellar inclination. In turn, we determine both the sky-projected (λ ≈ −0.4 ± 0.2◦) and true 3D obliquity (ψ ≈ 7+12 −4 ◦ ). We also find good agreement with the MHD simulations, with no significant centre-to-limb variations detectable in the local profiles. Hence, this technique provides a new powerful tool that can probe stellar photospheres, differential rotation, determine 3D obliquities, and remove sky-projection biases in planet migration theories. This technique can be implemented with existing instrumentation, but will become even more powerful with the next generation of high-precision radial velocity spectrographs.

Ultraviolet emission lines of Si II in cool star and solar spectra

Recent atomic physics calculations for Si II are employed within the CLOUDY modelling code to analyse Hubble Space Telescope (HST) STIS ultraviolet spectra of three cool stars, β Geminorum, α Centauri A and B, as well as previously published HST/GHRS observations of α Tau, plus solar quiet Sun data from the High Resolution Telescope and Spectrograph. Discrepancies found previously between theory and observation for line intensity ratios involving the 3s²3p ²PJ-3s3p^{2 4}P^J' intercombination multiplet of Si II at ~ 2335 Å are significantly reduced, as are those for ratios containing the 3s²3p ²PJ-3s3p^{2 2}DJ ~ transitions at ~1816 Å. This is primarily due to the effect of the new Si II transition probabilities. However, these atomic data are not only very different from previous calculations, but also show large disagreements with measurements, specifically those of Calamai et al. for the intercombination lines. New measurements of transition probabilities for Si II are hence urgently required to confirm (or otherwise) the accuracy of the recently calculated values. If the new calculations are confirmed, then a long-standing discrepancy between theory and observation will have finally been resolved. However, if the older measurements are found to be correct, then the agreement between theory and observation is simply a coincidence and the existing discrepancies remain.