36 research outputs found
Discovery of Radio Emission from the Brown Dwarf LP944-20
Brown dwarfs are classified as objects which are not massive enough to
sustain nuclear fusion of hydrogen, and are distinguished from planets by their
ability to burn deuterium. Old (>10 Myr) brown dwarfs are expected to possess
short-lived magnetic fields and, since they no longer generate energy from
collapse and accretion, weak radio and X-ray emitting coronae. Several efforts
have been undertaken in the past to detect chromospheric activity from the
brown dwarf LP944-20 at X-ray and optical wavelengths, but only recently an
X-ray flare from this object was detected. Here we report on the discovery of
quiescent and flaring radio emission from this source, which represents the
first detection of persistent radio emission from a brown dwarf, with
luminosities that are several orders of magnitude larger than predicted from an
empirical relation between the X-ray and radio luminosities of many stellar
types. We show in the context of synchrotron emission, that LP944-20 possesses
an unusually weak magnetic field in comparison to active dwarf M stars, which
might explain the null results from previous optical and X-ray observations of
this source, and the deviation from the empirical relations.Comment: Accepted to Natur
Surface features, rotation and atmospheric variability of ultra cool dwarfs
Photometric I band light curves of 21 ultra cool M and L dwarfs are
presented. Variability with amplitudes of 0.01 to 0.055 magnitudes (RMS) with
typical timescales of an hour to several hours are discovered in half of these
objects. Periodic variability is discovered in a few cases, but interestingly
several variable objects show no significant periods, even though the
observations were almost certainly sensitive to the expected rotation periods.
It is argued that in these cases the variability is due to the evolution of the
surface features on timescales of a few hours. This is supported in the case of
2M1145 for which no common period is found in two separate light curves. It is
speculated that these features are photospheric dust clouds, with their
evolution possibly driven by rotation and turbulence. An alternative
possibility is magnetically-induced surface features. However, chromospheric
activity undergoes a sharp decrease between M7 and L1, whereas a greater
occurrence of variability is observed in objects later than M9, lending support
to the dust interpretation.Comment: To appear in "Ultracool Dwarf Stars" (Lecture Notes in Physics),
H.R.A. Jones, I. Steele (eds), Springer-Verlag, 2001. Also available from
http://www.mpia-hd.mpg.de/homes/calj/ultra.htm
Radio Emission from Ultra-Cool Dwarfs
The 2001 discovery of radio emission from ultra-cool dwarfs (UCDs), the very
low-mass stars and brown dwarfs with spectral types of ~M7 and later, revealed
that these objects can generate and dissipate powerful magnetic fields. Radio
observations provide unparalleled insight into UCD magnetism: detections extend
to brown dwarfs with temperatures <1000 K, where no other observational probes
are effective. The data reveal that UCDs can generate strong (kG) fields,
sometimes with a stable dipolar structure; that they can produce and retain
nonthermal plasmas with electron acceleration extending to MeV energies; and
that they can drive auroral current systems resulting in significant
atmospheric energy deposition and powerful, coherent radio bursts. Still to be
understood are the underlying dynamo processes, the precise means by which
particles are accelerated around these objects, the observed diversity of
magnetic phenomenologies, and how all of these factors change as the mass of
the central object approaches that of Jupiter. The answers to these questions
are doubly important because UCDs are both potential exoplanet hosts, as in the
TRAPPIST-1 system, and analogues of extrasolar giant planets themselves.Comment: 19 pages; submitted chapter to the Handbook of Exoplanets, eds. Hans
J. Deeg and Juan Antonio Belmonte (Springer-Verlag
Theory of Low-Mass Stars and Substellar Objects
Since the discovery of the first bona-fide brown dwarfs and extra-solar
planets in 1995, the field of low mass stars and substellar objects has
considerably progressed, both from theoretical and observational
viewpoints.Recent developments in the physics entering the modeling of these
objects have led to significant improvements in the theory and to a better
understanding of their mechanical and thermal properties. This theory can now
be confronted with observations directly in various observational diagrams
(color-color, color-magnitude, mass-magnitude, mass-spectral type), a stringent
and unavoidable constraint which became possible only recently, with the
generation of synthetic spectra. In this paper, we present the current
state-of-the-art general theory of low-mass stars and sub-stellar objects, from
one solar mass to one Jupiter mass, regarding primarily their interior
structure and evolution. This review is a natural complement to the previous
review on the atmosphere of low-mass stars and brown dwarfs (Allard et al
1997). Special attention is devoted to the comparison of the theory with
various available observations. The contribution of low-mass stellar and
sub-stellar objects to the Galactic mass budget is also analysed.Comment: 81 pages, Latex file, uses aasms4.sty, review for Annual Review of
Astronomy and Astrophysics, vol. 38 (2000
A chemical survey of exoplanets with ARIEL
Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet’s birth, and evolution. ARIEL was conceived to observe a large number (~1000) of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25–7.8 μm spectral range and multiple narrow-band photometry in the optical. ARIEL will focus on warm and hot planets to take advantage of their well-mixed atmospheres which should show minimal condensation and sequestration of high-Z materials compared to their colder Solar System siblings. Said warm and hot atmospheres are expected to be more representative of the planetary bulk composition. Observations of these warm/hot exoplanets, and in particular of their elemental composition (especially C, O, N, S, Si), will allow the understanding of the early stages of planetary and atmospheric formation during the nebular phase and the following few million years. ARIEL will thus provide a representative picture of the chemical nature of the exoplanets and relate this directly to the type and chemical environment of the host star. ARIEL is designed as a dedicated survey mission for combined-light spectroscopy, capable of observing a large and well-defined planet sample within its 4-year mission lifetime. Transit, eclipse and phase-curve spectroscopy methods, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allow us to measure atmospheric signals from the planet at levels of 10–100 part per million (ppm) relative to the star and, given the bright nature of targets, also allows more sophisticated techniques, such as eclipse mapping, to give a deeper insight into the nature of the atmosphere. These types of observations require a stable payload and satellite platform with broad, instantaneous wavelength coverage to detect many molecular species, probe the thermal structure, identify clouds and monitor the stellar activity. The wavelength range proposed covers all the expected major atmospheric gases from e.g. H2O, CO2, CH4 NH3, HCN, H2S through to the more exotic metallic compounds, such as TiO, VO, and condensed species. Simulations of ARIEL performance in conducting exoplanet surveys have been performed – using conservative estimates of mission performance and a full model of all significant noise sources in the measurement – using a list of potential ARIEL targets that incorporates the latest available exoplanet statistics. The conclusion at the end of the Phase A study, is that ARIEL – in line with the stated mission objectives – will be able to observe about 1000 exoplanets depending on the details of the adopted survey strategy, thus confirming the feasibility of the main science objectives.Peer reviewedFinal Published versio
Formation, evolution and multiplicity of brown dwarfs and giant exoplanets
This proceeding summarises the talk of the awardee of the Spanish
Astronomical Society award to the the best Spanish thesis in Astronomy and
Astrophysics in the two-year period 2006-2007. The thesis required a tremendous
observational effort and covered many different topics related to brown dwarfs
and exoplanets, such as the study of the mass function in the substellar domain
of the young sigma Orionis cluster down to a few Jupiter masses, the relation
between the cluster stellar and substellar populations, the accretion discs in
cluster brown dwarfs, the frequency of very low-mass companions to nearby young
stars at intermediate and wide separations, or the detectability of Earth-like
planets in habitable zones around ultracool (L- and T-type) dwarfs in the solar
neighbourhood.Comment: "Highlights of Spanish Astrophysics V", Proceedings of the VIII
Scientific Meeting of the Spanish Astronomical Society (SEA) held in
Santander, 7-11 July, 2008. Edited by J. Gorgas, L. J. Goicoechea, J. I.
Gonzalez-Serrano, J. M. Diego. Invited oral contribution to plenary sessio
Variability of Brown Dwarfs
Brown dwarfs constitute a missing link between low-mass stars and giant
planets. Their atmospheres display chemical species typical of planets, and one
could wonder whether they also have weather-like patterns. While brown dwarf
surface features cannot be directly resolved, the photometric and spectroscopic
modulations induced by these features, as they rotate in and out of view,
provide a wealth of information on the evolution of their atmosphere. A review
of brown dwarfs variability through the L, T and Y spectral types sequence is
presented, as well as the constraints that they set on the nature of
weather-like patterns on their surface.Comment: Accepted chapter in the "Handbook of Exoplanets"; Springe
HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS
We report the discovery and characterization of a transiting warm sub-Neptune planet around the nearby bright (V = 8.75 mag, K = 7.15 mag) solar twin HD 183579, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located 56.8 ± 0.1 pc away with a radius of R* = 0.97 ± 0.02 R⊙ and a mass of M* = 1.03 ± 0.05 M⊙. We confirm the planetary nature by combining space and ground-based photometry, spectroscopy, and imaging. We find that HD 183579b (TOI-1055b) has a radius of Rp = 3.53 ± 0.13 R⊕ on a 17.47 d orbit with a mass of Mp = 11.2 ± 5.4 M⊕ (3σ mass upper limit of 27.4 M⊕). HD 183579b is the fifth brightest known sub-Neptune planet system in the sky, making it an excellent target for future studies of the interior structure and atmospheric properties. By performing a line-by-line differential analysis using the high-resolution and signal-to-noise ratio HARPS spectra, we find that HD 183579 joins the typical solar twin sample, without a statistically significant refractory element depletion
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images
We present the discovery and characterization of five hot and warm Jupiters—TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960)—based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (RP = 1.01–1.77 RJ) and have masses that range from 0.85 to 6.33 MJ. The host stars of these systems have F and G spectral types (5595 ≤ Teff ≤ 6460 K) and are all relatively bright (9.5 1.7 RJ, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of MJ and a statistically significant, nonzero orbital eccentricity of e = . This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals