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See detailL'astaxanthine: de la biologie à l'industrie
Fratamico, Anthony ULg

Scientific conference (2014, May 06)

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See detailAsteroid 45 Eugenia - Lightcurves and the pole orientation
Taylor, R. C.; Birch, P. V.; Pospieszalska-Surdej, Anna ULg et al

in ICARUS (1988), 73

Nine lightcurves of asteroid 45 Eugenia, three from 1969 and six from 1984, are given. In 1984 - 1985 the H[SUB]0[/SUB] magnitude of Eugenia, corrected to the lightcurve maximum, was 7.47 and the slope ... [more ▼]

Nine lightcurves of asteroid 45 Eugenia, three from 1969 and six from 1984, are given. In 1984 - 1985 the H[SUB]0[/SUB] magnitude of Eugenia, corrected to the lightcurve maximum, was 7.47 and the slope parameter G[SUB]0[/SUB] was 0.04. The north pole of Eugenia is within ±10° of ecliptic longitude 106° and latitude +26° (or 295° and +34°). This solution is consistent with an amplitude-aspect pole analysis. The sideral period is 0.2374645±0.0000002 day and the sense of rotation is retrograde. [less ▲]

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See detailAsteroid 532 Herculina - Lightcurves, pole orientation and a model
Taylor, R. C.; Birch, P. V.; Drummond, J. et al

in Icarus (1987), 69

Photoelectric lightcurves of 532 Herculina in 1984 show two maxima and two minima with a synodic rotation period of 0.39185±0.00002 day (1sigma). During some other oppositions the Herculina lightcurve has ... [more ▼]

Photoelectric lightcurves of 532 Herculina in 1984 show two maxima and two minima with a synodic rotation period of 0.39185±0.00002 day (1sigma). During some other oppositions the Herculina lightcurve has only one maximum and one minimum over that same rotation period. The absolute magnitude in V is 6.13±0.02 mag, the phase coefficient in V is 0.037±0.002, and the mean colors are B-V = +0.86±0.04 and U-B = +0.43±0.02. The authors applied photometric astrometry and the results indicate a sidereal period of 0.3918711±0.0000001 day with retrograde rotation for a north pole at 276° long and +1° lat. The uncertainty of the pole is ±1°. A model of Herculina is presented that generates lightcurves consistent with both the observed amplitudes and the timings of extrema over precisely 28,630 sidereal rotations during 30 years. [less ▲]

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See detailAsteroid lightcurves simulated by the rotation of a three-axes ellipsoid model
Surdej, Jean ULg; Surdej, Anna ULg

in Astronomy and Astrophysics (1978), 66

A triaxial-ellipsoid model is used to simulate the smooth and nearly symmetric light curves that are usually characteristic of asteroids which exhibit large brightness variations. The mathematical model ... [more ▼]

A triaxial-ellipsoid model is used to simulate the smooth and nearly symmetric light curves that are usually characteristic of asteroids which exhibit large brightness variations. The mathematical model is developed and applied to two problems involving an asteroid moving with its rotational axis either perpendicular to or lying within the plane containing the sun and earth. The numerical results obtained are compared with Dunlap's (1971) simulations of asteroid brightness variations, and it is argued that typical asteroid phase coefficients cannot be interpreted unambiguously. The results are shown to favor the Hapke-Irvine relation for describing the scattering properties of a dark asteroid surface. [less ▲]

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See detailAsteroid rotation - Hunting for a record: 1689 Floris-Jan
Schober, H. J.; Surdej, Jean ULg

in The Messenger (1982), 29

Last year, in June 1981 - ESO Messenger No. 24, p. 22-23 - H. J. Schober published areport on "Spinning Asteroids and Photometry". There he mainly gave a general introduction about what can be done using ... [more ▼]

Last year, in June 1981 - ESO Messenger No. 24, p. 22-23 - H. J. Schober published areport on "Spinning Asteroids and Photometry". There he mainly gave a general introduction about what can be done using UBV photometry in order to derive physical properties of asteroids such as geometrie forms, diameters, reflectance on the surface, bimodality of asteroids with respect to typology. A special effort was made to report about the activities to deal with asteroids as "variable objects" like variable stars - showing Iightcurves with defined rotation rates to be derived. Among asteroids it was stated that the longest rotation periods found before 1975 were not larger than 20 hours - followed by 654 Zelinda 31 ~9 (1975). 393 Lampetia 38h7, 128 Nemesis 39h0 (1979), 709 Fringilla 52h4 (1979) and 182 Eisa 80~00 (1980), the latter corresponding to 3d33. [less ▲]

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See detailASTEROID: regression de l'atherosclerose coronaire avec la rosuvastatine 'a une dose maximale de 40 mg par jour.
Scheen, André ULg

in Revue Médicale de Liège (2006), 61(4), 267-72

ASTEROID is a prospective, open-label blinded end-points trial aiming to assess whether very intensive statin therapy with rosuvastatin 40 mg/day could regress coronary atherosclerosis as determined by ... [more ▼]

ASTEROID is a prospective, open-label blinded end-points trial aiming to assess whether very intensive statin therapy with rosuvastatin 40 mg/day could regress coronary atherosclerosis as determined by intravascular ultrasound (IVUS). This multinational study included 507 patients, among whom 349 had evaluable serial IVUS examinations at 24 months. Rosuvastatin decreased LDL cholesterol level from 130 mg/dl to 61 mg/dl (- 53.2%) and increased HDL cholesterol from 43 to 49 mg/dl (+ 14.7%). The three prespecified IVUS efficacy parameters were positively altered by rosuvastatin, demonstrating regression of coronary atherosclerosis : the mean change in percent atheroma volume (- 0.98%), the change in atheroma volume in the most diseased 10-mm subsegment me (- 6.1 mm3) and the change in total atheroma volume (- 6.8%) were all significant (p < 0,001). Adverse events were infrequent and similar to other statin trials. The present study demonstrates that a 2-year treatment with a high dose of rosuvastatin 40 mg/day is able to induce significant regression of coronary atherosclerosis as determined by IVU imaging. Further ongoing studies in the GALAXY clinical investigation programme should now demonstrate that rosuvastatin, the most potent statin to reduce LDL and increase HDL cholesterol, is also able to diminish the incidence of clinical outcomes, cardiovascular events in general and major coronary events in particular. [less ▲]

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See detailThe asteroseismic analysis of the pulsating sdB Feige 48 revisited
Van Grootel, Valérie ULg; Charpinet, Stéphane; Fontaine, Gilles et al

Conference (2007, July)

We present a new detailed analysis of the short period pulsating sdB star Feige 48, based on the same observations than in our previous work (Charpinet et al., 2005, A&A 443, 251) but with our new codes ... [more ▼]

We present a new detailed analysis of the short period pulsating sdB star Feige 48, based on the same observations than in our previous work (Charpinet et al., 2005, A&A 443, 251) but with our new codes including the rotation of the star. Feige 48 is supposed to be a relatively fast rotator, showing a fine structure in its pulsation spectrum about 28 µHz on three groups in the 9 frequencies. On the other side, Feige 48 belongs to a close binary system (likely with a white dwarf) where the orbital period is 9.02 +/- 0.03h (S. O'Toole 2004). With our new codes including the rotation (for a given rotation law, we calculate associated multiplets for each frequency with the perturbative approach on the first order), avoiding us to make assumptions about the m=0 modes, we were able to fit all the 9 periods together, leading to sligthly different estimations for the structural parameters of Feige 48 than in our previous work. Moreover, the rotation of the star is found to be solid with a period of 32,540s <=> 9.038h, very close to the orbital period of the system determined by spectroscopy, confirming the reasonable assumption that the system is tidally locked. In this context, it was possible to exclude that Feige 48 has a fast rotating core in term of much poorer merit functions. [less ▲]

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See detailAn asteroseismic Main Sequence model for the delta Scuti star 44 Tau
Garrido, R.; Suárez, J. C.; Grigahcène, A. et al

in Communications in Asteroseismology (2007), 150

Not Available

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See detailAsteroseismic observations and modelling of 70 Ophiuchi AB
Eggenberger, P.; Miglio, Andrea ULg; Carrier, F. et al

in Journal of Physics Conference Series (2008), 118(1), 012053-

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See detailThe Asteroseismic Potential of Kepler: First Results for Solar-Type Stars
Chaplin, W. J.; Appourchaux, T.; Elsworth, Y. et al

in Astrophysical Journal Letters (2010), 713

We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise ... [more ▼]

We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: about 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses, and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe. [less ▲]

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See detailAsteroseismic probing of internal rotation in hot B subdwarf stars: Testing spin-orbit synchronism in two close binary systems
Van Grootel, Valérie ULg; Charpinet, Stéphane; Fontaine, Gilles et al

in Journal of Physics: Conference Series (2009, June), 172

We present internal rotation profiles derived from asteroseismology for the hot pulsating B subdwarf stars PG 1336-018 and Feige 48. These two pulsators are primaries of close binary systems of known ... [more ▼]

We present internal rotation profiles derived from asteroseismology for the hot pulsating B subdwarf stars PG 1336-018 and Feige 48. These two pulsators are primaries of close binary systems of known orbital period and, therefore, provide laboratories to test, for the first time, spin-orbit synchronization as a function of depth. We show that PG 1336-018 and Feige 48 clearly rotate as solid bodies with periods equal to their orbital periods from the surface down to at least ~ 0.5 and ~ 0.3 their radius, respectively. Deep tidal locking has therefore developed within the relatively short lifetime of these stars (~ 10^8 yr). [less ▲]

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See detailAsteroseismic Solutions for the Two Fast Subdwarf B Pulsators Balloon 090100001 and PG 1336-018
Charpinet, Stéphane; Van Grootel, Valérie ULg; Brassard, Pierre et al

in Leaflet - Astronomical Society of the Pacific (2008, January), 392

We present two new asteroseismic studies of the rapid sdB pulsator PG 1336-018 and the hybrid sdB pulsator Balloon (BAL) 090100001. For PG 1336-018, the analysis is based on 25 periods extracted from the ... [more ▼]

We present two new asteroseismic studies of the rapid sdB pulsator PG 1336-018 and the hybrid sdB pulsator Balloon (BAL) 090100001. For PG 1336-018, the analysis is based on 25 periods extracted from the white-light photometry of the Xcov17 Whole Earth Telescope campaign (Kilkenny et al. 2003). For BAL 090100001, we use 10 periods of high amplitudes for which constraints on the ℓ-index have been derived from high S/N multicolour photometry. From asteroseismology, we estimate important structural parameters for these two stars, including the stellar mass and the H-rich envelope thickness. The analyses presented here are of particular interest since the asteroseismic results can be tested using independent constraints, which confirm the robustness of the solutions in both cases. [less ▲]

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See detailAn asteroseismic study of the beta Cephei CoRoT main target HD 180642: results from the ground-based campaign
Briquet, Maryline ULg; Uytterhoeven, K.; Morel, Thierry ULg et al

in American Institute of Physics Conference Series (2009, September 01)

The β Cephei star HD 180642 was observed by the CoRoT satellite during a run of 156 days in 2007. The space white light photometry revealed the rich frequency spectrum of the star (Degroote et al. 2009 ... [more ▼]

The β Cephei star HD 180642 was observed by the CoRoT satellite during a run of 156 days in 2007. The space white light photometry revealed the rich frequency spectrum of the star (Degroote et al. 2009). In the present study, we provide additional information on the target, based on both ground-based multi-colour photometry and high-resolution spectroscopy. We place our object in the (T[SUB]eff[/SUB], log g) diagram. In addition, we derive the chemical abundances of several elements as well as the metallicity of HD 180642. Finally, we put constraints on the identification of some modes. All these observational constraints will be used to compute stellar models of the target. [less ▲]

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See detailAn asteroseismic study of the beta Cephei star beta Canis Majoris
Desmet, M.; Briquet, Maryline ULg; Mazumdar, A. et al

in Communications in Asteroseismology (2006), 147

We present a spectroscopic study of the beta Cephei star beta Canis Majoris. Hundreds of high-resolution spectra were gathered during 4.5 years and the Si III line profiles centered on 4560 A were ... [more ▼]

We present a spectroscopic study of the beta Cephei star beta Canis Majoris. Hundreds of high-resolution spectra were gathered during 4.5 years and the Si III line profiles centered on 4560 A were subjected to a detailed line profile analysis. We searched for oscillation frequencies in different line diagnostics, compared them with those known from photometric studies and concluded the presence of three frequencies in our dataset: f_1 = 3.97933 c/d, f_2 = 3.99959 c/d and f_3= 4.1832 c/d, which were already found earlier from photometric data. By means of the moment method and from amplitude and phase variations across the profiles we could identify two of the modes as (l_1,m_1)=(2,2) and (l_2,m_2)=(0,0$. We present our first results of modelling based on the oscillation frequencies and place constraints on the mass, age and core overshooting of this massive evolved beta Cephei star. [less ▲]

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See detailAn asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry
Briquet, Maryline ULg; Aerts, C.; Baglin, A. et al

in Astronomy and Astrophysics (2011), 527

The O9V star HD 46202, which is a member of the young open cluster NGC 2244, was observed by the CoRoT satellite in October/November 2008 during a short run of 34 days. From the very high-precision light ... [more ▼]

The O9V star HD 46202, which is a member of the young open cluster NGC 2244, was observed by the CoRoT satellite in October/November 2008 during a short run of 34 days. From the very high-precision light curve, we clearly detect β Cep-like pulsation frequencies with amplitudes of ~0.1 mmag and below. A comparison with stellar models was performed using a χ[SUP]2[/SUP] as a measure for the goodness-of-fit between the observed and theoretically computed frequencies. The physical parameters of our best-fitting models are compatible with the ones deduced spectroscopically. A core overshooting parameter α[SUB]ov[/SUB] = 0.10 ± 0.05 pressure scale height is required. None of the observed frequencies are theoretically excited with the input physics used in our study. More theoretical work is thus needed to overcome this shortcoming in how we understand the excitation mechanism of pulsation modes in such a massive star. A similar excitation problem has also been encountered for certain pulsation modes in β Cep stars recently modelled asteroseismically. The CoRoT space mission was developed and is operated by the French space agency CNES, with the participation of ESA's RSSD and Science Programmes, Austria, Belgium, Brazil, Germany, and Spain. [less ▲]

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See detailAn asteroseismic study of the β Cephei star 12 Lacertae: multisite spectroscopic observations, mode identification and seismic modelling
Desmet, M.; Briquet, Maryline ULg; Thoul, Anne ULg et al

in Monthly Notices of the Royal Astronomical Society (2009), 396

We present the results of a spectroscopic multisite campaign for the β Cephei star 12 (DD) Lacertae. Our study is based on more than thousand high-resolution high S/N spectra gathered with eight different ... [more ▼]

We present the results of a spectroscopic multisite campaign for the β Cephei star 12 (DD) Lacertae. Our study is based on more than thousand high-resolution high S/N spectra gathered with eight different telescopes in a time span of 11 months. In addition, we make use of numerous archival spectroscopic measurements. We confirm 10 independent frequencies recently discovered from photometry, as well as harmonics and combination frequencies. In particular, the slowly pulsating B-stars (SPB)-like g-mode with frequency 0.3428d[SUP]-1[/SUP] reported before is detected in our spectroscopy. We identify the four main modes as (l[SUB]1[/SUB], m[SUB]1[/SUB]) = (1, 1), (l[SUB]2[/SUB], m[SUB]2[/SUB]) = (0, 0), (l[SUB]3[/SUB], m[SUB]3[/SUB]) = (1, 0) and (l[SUB]4[/SUB], m[SUB]4[/SUB]) = (2, 1) for f[SUB]1[/SUB] = 5.178964d[SUP]-1[/SUP], f[SUB]2[/SUB] = 5.334224d[SUP]-1[/SUP], f[SUB]3[/SUB] = 5.066316d[SUP]-1[/SUP] and f[SUB]4[/SUB] = 5.490133d[SUP]-1[/SUP], respectively. Our seismic modelling shows that f[SUB]2[/SUB] is likely the radial first overtone and that the core overshooting parameter α[SUB]ov[/SUB] is lower than 0.4 local pressure scale heights. [less ▲]

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See detailAn asteroseismic study of the β Cephei star β Canis Majoris
Mazumdar, A.; Briquet, Maryline ULg; Desmet, M. et al

in Astronomy and Astrophysics (2006), 459

Aims.We present the results of a detailed analysis of 452 ground-based, high-resolution high S/N spectroscopic measurements spread over 4.5 years for β Canis Majoris with the aim of determining the ... [more ▼]

Aims.We present the results of a detailed analysis of 452 ground-based, high-resolution high S/N spectroscopic measurements spread over 4.5 years for β Canis Majoris with the aim of determining the pulsational characteristics of this star, and then using them to derive seismic constraints on the stellar parameters.<BR /> Methods: .We determined pulsation frequencies in the Si III 4553 Å line with Fourier methods. We identified the m-value of the modes by taking the photometric identifications of the degrees ℓ into account. To this end we used the moment method together with the amplitude and phase variations across the line profile. The frequencies of the identified modes were used for a seismic interpretation of the structure of the star.<BR /> Results: .We confirm the presence of the three pulsation frequencies already detected in previous photometric datasets: f[SUB]1[/SUB] = 3.9793~c d[SUP]-1[/SUP] (46.057~μHz), f[SUB]2[/SUB] = 3.9995~c d[SUP]-1[/SUP] (46.291~μHz), and f[SUB]3[/SUB] = 4.1832~c d[SUP]-1[/SUP] (48.417~μHz). For the two modes with the highest amplitudes, we unambiguously identify (ℓ_1,m_1) = (2,2) and (ℓ_2,m_2) = (0,0). We cannot conclude anything for the third mode identification, except that m[SUB]3[/SUB] > 0. We also deduce an equatorial rotational velocity of 31 ± 5~km s[SUP]-1[/SUP] for the star. We show that the mode f[SUB]1[/SUB] must be close to an avoided crossing. Constraints on the mass (13.5 ± 0.5~μHz), age (12.4 ± 0.7 Myr), and core overshoot (0.20 ± 0.05 H_P) of β CMa are obtained from seismic modelling using f[SUB]1[/SUB] and f_2.<BR /> [less ▲]

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See detailAn asteroseismic study of the β cephei star θ ophiuchi : constraints on global stellar parameters and core overshooting
Briquet, Maryline ULg; Morel, Thierry ULg; Thoul, Anne ULg et al

in Monthly Notices of the Royal Astronomical Society (2007), 381(4), 1482-1488

We present a seismic study of the beta Cephei star theta Ophiuchi. Our analysis is based on the observation of one radial mode, one rotationally split l = 1 triplet and three components of a rotationally ... [more ▼]

We present a seismic study of the beta Cephei star theta Ophiuchi. Our analysis is based on the observation of one radial mode, one rotationally split l = 1 triplet and three components of a rotationally split l = 2 quintuplet for which the m values were well identified by spectroscopy. We identify the radial mode as fundamental, the triplet as p(1) and the quintuplet as g(1). Our non-local thermodynamic equilibrium abundance analysis results in a metallicity and CNO abundances in full agreement with the most recent updated solar values. With X epsilon [0.71, 0.7211] and Z epsilon [0.009, 0.015], and using the Asplund et al. mixture but with a Ne abundance about 0.3 dex larger, the matching of the three independent modes enables us to deduce constrained ranges for the mass (M = 8.2 +/- 0.3 M circle dot) and central hydrogen abundance (X-c = 0.38 +/- 0.02) of theta Oph and to prove the occurrence of core overshooting (alpha(ov) = 0.44 +/- 0.07). We also derive an equatorial rotation velocity of 29 +/- 7 km s(-1). Moreover, we show that the observed non-equidistance of the l = 1 triplet can be reproduced by the second-order effects of rotation. Finally, we show that the observed rotational splitting of two modes cannot rule out a rigid rotation model. [less ▲]

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See detailAn asteroseismic study of the β Cephei star θ Ophiuchi: spectroscopic results
Briquet, Maryline ULg; Lefever, K.; Uytterhoeven, K. et al

in Monthly Notices of the Royal Astronomical Society (2005), 362

We present the results of a detailed analysis of 121 ground-based high-resolution, high signal-to-noise ratio spectroscopic measurements spread over 3 yr for the β Cephei star θ Ophiuchi. We discovered θ ... [more ▼]

We present the results of a detailed analysis of 121 ground-based high-resolution, high signal-to-noise ratio spectroscopic measurements spread over 3 yr for the β Cephei star θ Ophiuchi. We discovered θ Oph to be a triple system. In addition to the already known speckle B5 companion of the B2 primary, we showed the presence of a low-mass spectroscopic companion and we derived an orbital period of 56.71 d with an eccentricity of 0.1670. After removing the orbit we determined two frequencies for the primary in the residual radial velocities: f[SUB]1[/SUB]= 7.1160 cd[SUP]-1[/SUP] and f[SUB]2[/SUB]= 7.4676 cd[SUP]-1[/SUP]. We also found the presence of f[SUB]3[/SUB]= 7.3696 cd[SUP]-1[/SUP] by means of a two-dimensional frequency search across the SiIII 4567-Åprofiles. We identified the m-value of the main mode with frequency f[SUB]1[/SUB] by taking into account the photometric identifications of the degrees l. By means of the moment method and the amplitude and phase variations across the line profile, we derived (l[SUB]1[/SUB], m[SUB]1[/SUB]) = (2, -1). This result allows us to fix the mode identifications of the whole quintuplet for which three components were detected in photometry. This is of particular use for our forthcoming seismic modelling of the primary. We also determined stellar parameters of the primary by non-local thermodynamic equilibrium hydrogen, helium and silicon line profile fitting and we obtained T[SUB]eff[/SUB]= 24000 K and logg= 4.1, which is consistent with photometrically determined values. [less ▲]

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See detailAn Asteroseismological Analysis of the Pulsating B Subdwarf Feige 48 Taking into Account Rotation
Van Grootel, Valérie ULg; Charpinet, Stéphane; Fontaine, Gilles et al

in Leaflet - Astronomical Society of the Pacific (2008, January), 392

We present a new analysis of the short period pulsating sdB star Feige 48 using the same observations as done in our previous work, but exploiting, this time, our new period-matching codes that include ... [more ▼]

We present a new analysis of the short period pulsating sdB star Feige 48 using the same observations as done in our previous work, but exploiting, this time, our new period-matching codes that include the rotation of the star. The pulsation spectrum of Feige 48 shows the signature of rotational splitting with a mean frequency spacing of about 28 μHz between the components of three different frequency multiplets. In addition, Feige 48 has been shown to be a member of a close binary system with an invisible (most likely a white dwarf) companion. Assuming various internal rotation laws, we are now able to fit all nine observed frequencies simultaneously, and not only the four m = 0 components that we identified a priori in our previous effort. For solid body rotation, our optimal model shows slightly different structural parameters than those obtained previously on the basis of purely spherical models. Interestingly, that optimal model is also characterized by a rotation period of 9.028 h, which falls exactly on the value of the orbital period found independently from spectroscopy, namely, 9.024 ± 0.072 h. This very strongly implies that Feige 48 is tidally locked, a suggestion quite consistent with theoretical expectations for such a close binary system. In the same vein, our investigations also demonstrate explicitly that the idea of a fast rotating core can be eliminated for Feige 48. [less ▲]

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