Issue |
A&A
Volume 507, Number 2, November IV 2009
|
|
---|---|---|
Page(s) | 881 - 889 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/200911641 | |
Published online | 27 August 2009 |
A&A 507, 881-889 (2009)
EX Lupi in quiescence![[*]](/icons/foot_motif.png)
N. Sipos1 - P. Ábrahám1 - J. Acosta-Pulido2 - A. Juhász3 - Á. Kóspál4 - M. Kun1 - A. Moór1 - J. Setiawan3
1 - Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, 1525
Budapest, Hungary
2 -
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Canary Islands, Spain
3 -
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
4 -
Leiden Observatory, Leiden University, PO Box 9513, 2300RA Leiden, The Netherlands
Received 9 January 2009 / Accepted 4 June 2009
Abstract
Aims. EX Lupi is the prototype of EXors, a subclass of
low-mass pre-main sequence stars whose episodic eruptions are
attributed to temporarily increased accretion. In quiescence the
optical and near-infrared properties of EX Lup cannot be
distinguished from those of normal T Tau stars. Here we investigate
whether it is the circumstellar disk structure that makes EX Lup
an atypical Class II object. During outburst the disk might
undergo structural changes. Our characterization of the quiescent disk
is intended to serve as a reference for studying the physical changes
related to one of EX Lupi's strongest known eruptions in 2008
Jan-Sep.
Methods. We searched the literature for photometric and
spectroscopic observations including ground-based, IRAS, ISO, and
Spitzer data. After constructing the optical-infrared spectral energy
distribution (SED), we compared it with the typical SEDs of other young
stellar objects and modeled it using the Monte Carlo radiative transfer
code RADMC. We determined the mineralogical composition of the 10 m silicate emission feature and also gave a description of the optical and near-infrared spectra.
Results. The SED is similar to that of a typical T Tauri star in most aspects, though EX Lup emits higher flux above 7 m.
The quiescent phase data suggest low-level variability in the
optical-mid-infrared domain. By integrating the optical and infrared
fluxes, we derived a bolometric luminosity of 0.7
.
The 10
m
silicate profile could be fitted by a mixture consisting of amorphous
silicates, but no crystalline silicates were found. A modestly flaring
disk model with a total mass of 0.025
and an outer radius of 150 AU was able to reproduce the observed
SED. The derived inner radius of 0.2 AU is larger than the
sublimation radius, and this inner gap sets EX Lup apart from
typical T Tauri stars.
Key words: stars: formation - stars: circumstellar matter - stars: individual: EX Lup - infrared: stars
1 Introduction
In 2008 January the amateur astronomer A. Jones announced that EX Lupi, the
prototype of the EXor class of pre-main sequence eruptive variables, had brightened
dramatically (Jones 2008). The quiescent phase brightness of EX Lup,
an M0 V star in the Lupus 3 star-forming region, is
mag.
During its unpredictable flare-ups, its brightness may increase by 1-5 mag for a period of several months (Herbig 1977). In past decades EX Lup produced a number of eruptions, the last one in 2002 (Herbig 2007,1977; Herbig et al. 2001). During the present outburst, which lasted
until 2008 September (AAVSO International Database
),
EX Lup reached a peak brightness of 8 mag in 2008 January,
brighter than ever before.
According to the current paradigm, eruptive phenomena in pre-main sequence stars
(FU Ori and EX Lup-type outbursts) are caused by enhanced accretion onto the central
star. Intense build-up of the stellar mass takes place during these phases of the star formation process
(Hartmann & Kenyon 1996).
In this picture circumstellar matter must play a crucial role in the
eruption mechanism. Surprisingly little is known about the
circumstellar environment of the EXor prototype, EX Lup. While its
infrared excess emission
detected by IRAS and ISO was attributed to a circumstellar disk (Gras-Velázquez & Ray 2005),
no detailed analysis or modeling of the disk structure has been
performed so far. Such an analysis could contribute to clarifying the
eruption mechanism and also answering the longstanding open question of
what distinguishes EXors from normal T Tau stars.
Herbig (2008) found no optical spectroscopic features that would uniquely define EXors, and
he also concluded that their location in the (J-H) vs.
color-color diagram
coincides with the domain occupied by T Tau stars.
In this work we search the literature and construct a complete optical-infrared spectral energy distribution (SED) of EX Lup that is representative of the quiescent phase. The SED is modeled using a radiative transfer code and will be compared with typical SEDs of T Tau stars, in order to reveal differences possibly defining the EXor class. During the recent extreme eruption, EX Lupi was observed with a wide range of instruments. Our results on the physical parameters of the system can be used as a reference for evaluating the changes related to this outburst.
2 Optical / infrared data
2.1 Optical and near-infrared photometry from the literature
We searched the literature and collected available optical and near-infrared photometric observations of EX Lup obtained during its quiescent phase. We defined quiescence periods as when the source was fainter than 12.5 mag according to the visual estimates and V-band magnitudes in the AAVSO International Database. A visual inspection of the DSS and the 2MASS images revealed no nebulosity surrounding the star, so we concluded that measurements taken with different apertures can be safely compared. The query results are presented in Table 1 and plotted in Fig. 1.
Table 1: Optical and infrared observations of EX Lup collected from the literature, obtained in its quiescent periods.
2.2 ESO 2.2/FEROS optical spectroscopy
Three spectra of EX Lup in quiescent phase were taken in 2007 July with FEROS at the 2.2 m MPG/ESO telescope in ESO La Silla, Chile. FEROS has a spectral resolution of 48 000 and a wavelength coverage from 360 to 920 nm (Kaufer et al. 1999). The data was reduced using the online FEROS Data Reduction System implemented on the telescope, which produced 39 one dimensional spectra of echelle orders and a merged spectrum of the entire wavelength range.
With a cross-correlation method, we computed the projected rotational
velocity and radial velocity of EX Lup in quiescence from the FEROS
spectra.
We cross-correlated the spectra with a numerical template
mask (Baranne et al. 1996). The mean
radial velocity is
km s-1. From the B-V color of EX Lup and by using a projected rotational velocity calibration for FEROS
(Setiawan et al. 2004), we derived a
km s-1. Sections of the spectrum showing the most prominent emission lines are plotted in Fig. 2.
2.3 NTT/SOFI near-infrared spectroscopy
We found near-IR spectra in the ESO Data Archive, obtained on
2001 May 4 using SOFI at the ESO 3.5 m NTT
telescope, under the program 67.C-0221(A) (PI:D. Folha). Two spectra
were taken using the blue and red grisms (
), which
cover the ranges
0.95-1.64 and
1.53-2.52
m, respectively. In both cases, the total
exposure time was 500 s, divided into 4 exposures following an
ABBA nodding pattern. The data were reduced using our dedicated routines
developed in the IRAF environment. The data reduction included
sky-subtraction, wavelength-calibration, and frame combination.
Spectra of the G3V star HIP 78466 were used to correct for telluric absorption.
A modified version of the Xtellcor software (Vacca et al. 2003) was used in this step. The spectrum is presented in Fig. 3.
2.4 InfraRed Astronomical Satellite (IRAS)
EX Lup is included in the IRAS Point Source Catalog with detections at 12, 25 and 60


![[*]](/icons/foot_motif.png)
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Figure 1:
Spectral energy distribution of EX Lup, showing all data points
from Tables 1 and 2 and the smoothed spectra obtained with
NTT/SOFI, ISOPHOT-S, and Spitzer/IRS. The gray stripe marks the median
SED of T Tauri objects from the Taurus-Auriga star-forming region.
The 5-36 |
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![]() |
Figure 2:
Details of the optical spectrum of EX Lupi showing significant or
typical features. The interval shown in the second panel of the upper row is
the same as Herbig's (2007) Fig. 3. It is apparent that the
broad component of the Fe II |
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2.5 Infrared Space Observatory (ISO)
EX Lup was observed on 5 dates with ISOPHOT, the photometer
onboard ISO (Lemke et al. 1996).
Four measurements belong to a small monitoring
program that adopted similar instrumental setups at each epoch (PI: T.
Prusti). For such datasets, an algorithm aimed to achieve high relative
photometry accuracy was developed in our group
(Juhász et al. 2007).
The raw data were corrected for instrumental effects following the scheme described in Juhász et al. (2007). Absolute flux calibration was performed by using the onboard
calibration source (FCS) for the 3.6-12 m filters and by assuming a default responsivity for the 20-25
m range. At different single epochs 60, 100, and 200
m high-resolution maps were
performed using the Astronomical Observing Template P32. These data were
processed using a dedicated P32 Tool (Tuffs & Gabriel 2003) and the calibration used the related FCS measurements.
The flux values were color-corrected by convolving the SED of EX Lup with
the ISOPHOT filter profiles. The results are listed in Table 2,
where the quoted formal uncertainties correspond to a conservative
estimate of 15%; however, the measurement error above 25
m is probably higher than this value.
The fifth photometric dataset was published by Gras-Velázquez & Ray (2005), but these data will not be used in our analysis due to their presumably higher uncertainties.
At the four epochs of the monitoring program low-resolution spectrophotometry was also performed
with the ISOPHOT-S sub-instrument in the 2.5-11.6 m wavelength range. These observations were reduced following the
processing scheme described by
Kóspál et al. (2009a, in prep.), which corrected for the slight
off-center positioning of the source, subtracted the separate
background spectra, and adopted realistic error bars. The processed and
calibrated spectra are shown in Fig. 1.
Table 2: Color-corrected fluxes of EX Lupi*.
2.6 Spitzer Space Telescope
IRAC.
EX Lup was observed with IRAC at 3.6, 4.5, 5.8, and 8.0


![]() |
Figure 3: Near-infrared spectrum of EX Lupi, observed on 2001 May 4. The region around the 12CO bandhead absorption is enlarged in the inset. |
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IRS.
EX Lup was observed with the Infrared Spectrograph (IRS, Houck et al. 2004) of the Spitzer
Space Telescope on 2004 Aug. 30 (PID: 172, PI: N. Evans) and on 2005 March 18 (PID:3716,
PI: G. Stringfellow). On the first date, the target was measured using Short Low (5.2-14.5 m),
Long Low (14.0-38
m), Short High (9.9-19.5
m), and Long High (18.7-37.2
m)
modules. The integration time was 14 s for the low-resolution modules, while 30 s and 60 s
were used for the Short High and Long High modules, respectively.
At the second epoch only the Short Low, Short High, and Long High modules were used and
a PCRS peak-up was executed prior to the spectroscopic observation to acquire the target in the
spectrograph slit. The integration times were 14 s for the Short Low module with 4 observing
cycles for redundancy, while 120 s and 60 s were used for the Short High and Long High modules,
respectively, both with 2 observing cycles.
The spectra are based on the droopres and rsc products processed through the S 15.3.0 version
of the Spitzer
data pipeline for the low- and high-resolution data, respectively. For
the low-resolution spectra, the background was subtracted using
associated pairs of imaged spectra from the two nodded positions, also
eliminating stray light
contamination and anomalous dark currents. For the high-resolution
spectra, the background was removed by fitting a local continuum
underneath the source profile. Pixels flagged by the
data pipeline as being ``bad'' were replaced with a value interpolated
from an 8 pixel perimeter
surrounding the flagged pixel. The spectra were extracted using a
6.0 pixel and 5.0 fixed-width aperture in the spatial dimension
for the Short Low and the Long Low modules, respectively, while
in the case of the high-resolution modules the spectra were extracted
by fitting the source profile
with the known PSF in the spectral images. The low-level fringing at
wavelengths >20 m was
removed using the irsfringe package (Lahuis & Boogert 2003). The spectra were calibrated with a
spectral response function derived from IRS spectra and MARCS stellar models for a suite of
calibrators provided by the Spitzer Science Center. To remove any effect of pointing offsets,
we matched orders based on the point spread function of the IRS instrument, correcting for
possible flux losses.
The spectra obtained at the two different dates agree within an uncertainty of
and are shown in Fig. 1.
3 Results
3.1 Variability in the quiescent phase
The observations of EX Lup are sporadic, so no complete SED could
be constructed for any given epoch. We decided to merge all quiescent
data regardless of their dates.
In Fig. 1 we plotted all
fluxes listed in Tables 1 and 2.
At most wavelengths, the scatter of data points is on the order of 25%,
though at optical and a few mid-infrared wavelengths, the difference
between the lowest and highest values can be considerably larger. The
ISOPHOT-S and Spitzer spectra shown in Fig. 1
also exhibit differences at similar levels. Although part of this
scatter is related to instrumental and calibration effects, the
individual error bars are typically much smaller than the scatter of
the data points, strongly suggesting the existence of an intrinsic
variability. However, in the case of the 60 and 100 m
data points, the uncertainty of the measurements is much higher than at
shorter wavelengths, so here the difference between the fluxes is
within the error bars. We consider the 25% peak-to-peak variation as an
upper limit for the variability of EX Lup in quiescence. According
to
Fig. 1, the variability might be somewhat greater at
optical wavelengths, but the low number of data points prevents
us from claiming a wavelength dependence.
Table 3: Observed wavelength, EW, and FWHM of the most prominent emission lines in the optical spectrum of EX Lupi in quiescence*.
3.2 The optical-infrared SED
The measured SED of EX Lup is presented in Fig. 1.
The optical part is clearly dominated by the stellar photosphere. The optical and near-infrared
colors, however differ slightly from the standard colors of an M0 V star.
This fact has already been mentioned by Gras-Velázquez & Ray (2005), who could not derive a positive extinction value from the EB-V and ER-I colors. Similarly, Herbig et al. (2001) claim it is unknown as well.
An infrared excess above the photosphere is detectable
longwards of the K-band. The 3-8 m
range is smooth and devoid of any
broad spectral features, indicating that EX Lup is neither deeply
embedded to exhibit ices nor hot enough to excite PAHs. A strong
silicate emission appears at 10
m, and a
corresponding - though broader and shallower - silicate band can be
seen around 20
m. At longer wavelengths, the continuum
emission decreases following a power law with a spectral index
of about -4/3. The lack of any sub-mm
or mm measurement means that the SED cannot be followed longwards of 200
m.
3.3 Spectroscopy
3.3.1 The optical spectrum
The high-resolution optical spectrum of EX Lupi, obtained on 2007 July 30, shows several emission lines in addition to the photospheric absorption features characteristic of the young late-type star. The emission lines are mostly symmetric, without noticeable P Cygni or inverse P Cygni absorption. The most prominent emission lines are the Balmer lines of the hydrogen, the H and K lines and the infrared triplet of the ionized calcium, and the helium lines at 5875 and 6678 Å. The observed wavelengths and equivalent widths in Å and the full widths at half maximum in km s-1, determined by Gaussian fitting, are listed in Table 3. In addition to these prominent features, more than 200 weak, narrow metallic lines could be identified using Moore's (1945) multiplet tables. The widths of the lines are around 10-20 km s-1, indicating that they originate in the active chromosphere of the star (Hamann & Persson 1992). All the emission lines identified in the spectrum are listed in the electronic version of Table 3 at the Centre de Données astronomiques de Strasbourg (CDS). Figure 2 shows sections of the spectrum.
The shape of the H line is nearly symmetric. Its equivalent width,
W(H
35.9 Å, is significantly larger than the upper
limit of the chromospheric H
emission of M0 type stars
(
6
,
Barrado y Navascués & Martín 2003), indicating
active accretion during the quiescent phase. The velocity width of the
H
line 10% above the continuum level is 362 km s-1,
larger than the lower limit of 270 km s-1, set by White & Basri
(2003) for accreting T Tauri stars.
The empirical relationship between the 10% width of the H
line
and the accretion rate
,
found by Natta et al. (2004),
allowed us to derive
yr.
Comparison of the H
line with the one published by Reipurth,
Pedrosa & Lago (1996) shows that in 2007 the H
emission line
of EX Lupi was more symmetric narrower and had somewhat larger equivalent
width than in 1994 March, a few days after an outburst.
3.3.2 Near-infrared spectrum
The flux-calibrated infrared spectrum, observed on 2001 May 4, is displayed in
Fig. 3. The shape of the spectrum is similar to that of an
unreddened M-type star without near-infrared excess (Greene & Lada 1996).
In the ZJ band the Paschen ,
,
,
and the
He I
1.083
m lines are seen in emission.
Absorption features of the Na I at 2.21
m,
Ca I at 2.26
m, and the rovibrational
transitions
of CO at 2.3-2.4
m can be identified in the
K-band part of the spectrum. The Br
line of the hydrogen is
barely visible in emission, but its equivalent width cannot be
measured. The following absorption features are also identified in our spectrum:
at 1.199
m a very deep feature corresponding to S I; at 1.577
m a
feature associated to Mg I, and at 1.673
m another feature associated with
Al I.
The Pa
emission line is a useful accretion tracer, because its luminosity
correlates well with the accretion luminosity (e.g. Muzerolle et al. 1998;
Dahm 2008). We used the relationship established by Muzerolle et al. (1998) to
derive the accretion luminosity of EX Lup during quiescence from the
measured flux F(Pa
W m-2. The resulting
allowed us to determine the
mass accretion rate
,
taking the mass and the radius
of the star from Table 6. The accretion was assumed to proceed through a gaseous disk; for its inner radius we adopted
(Gullbring et al. 1998).
The result is
/yr,
in agreement with
obtained from the
velocity width of the H
line.
A flux calibration uncertainty of 20% and the uncertainty
of the empirical relationship sets the lower and upper limits at
/yr and
/yr,
respectively.
4 Discussion
4.1 Comparison with young stellar objects
Infrared SEDs of eruptive young stars (EXors and/or FUors) were examined by Green et al. (2006), Quanz et al. (2007) and Kóspál et al. (2009b, in prep.).
Some of these stars (eg. UZ Tau, VY Tau,
DR Tau, FU Ori, Bran 76) resemble
EX Lupi. Their SEDs decrease towards longer wavelengths and show a
silicate feature in emission. The SEDs of the other group of FU
Ori-type or EXor-like variables (e.g. V1057 Cyg,
V1647 Ori, PV Cep, OO Ser) exhibit flat
or increasing SEDs in the 20-100 m wavelength range (Kóspál et al. 2007; Ábrahám et al. 2004), which is clearly different from the shape of EX Lupi's spectral energy distribution. Green et al. (2006) and Quanz et al. (2007)
suggest that the diversity in the shape of the SEDs is related to the
evolution of the system. Younger objects, still embedded in a large
envelope exhibit flat SEDs, while more evolved objects, emitting
T Tauri-like SEDs have already lost their envelopes and only have
circumstellar disks. According to this categorization we conclude that
EX Lupi is relatively evolved among eruptive stars, and expect
that its circumstellar environment only consists of a disk without an
envelope.
To compare EX Lup with other - not eruptive - young stars, in Fig. 1 we overplotted a gray stripe marking the median SED of T Tauri objects from the Taurus-Auriga star-forming region (D'Alessio et al. 1999; Furlan et al. 2006).
The SED of EX Lupi follows the Taurus median at shorter wavelengths. Longwards of approximately 7 m, however, its absolute level becomes higher than the median by a factor of
2.5. Nevertheless, even in this longer wavelength range its shape still resembles the Taurus slope.
Another comparison of EX Lupi with other pre-main sequence stars can be based on the mid-infrared spectrum. Furlan et al. (2006)
present a large sample of Spitzer IRS spectra of young stars and group
them into several categories by measuring the slope of the SEDs and the
strength of the 10 and 20 m
silicate features. A visual classification places EX Lup in their
scheme in group A or in group B, defined by a relatively strong
silicate feature and a flat or somewhat decreasing SED over 20
m. Furlan et al. (2006)
suggest that only limited dust-growth and settling has taken place in
these groups. Nonetheless, we find that EX Lup is not a typical
member of these groups, since shortwards of 8
m
the steep decrease of excess emission characteristic of their objects
is missing in the case of EX Lupi. These qualitative conclusions
can be verified by calculating color indices for EX Lup. The
strength of its silicate feature
is an intermediate value between group A and group B objects. However, the n6-25
spectral index is typically negative for all objects in the sequence
while positive (0.03) in the case of EX Lupi, making it an
``outlier'' in the scheme. Also, the correlation between the n6-13 and n13-25 indices found by Furlan et al. (2006)
does not seem to hold for EX Lup. The colors of IRAS 04385+2550, a
star exhibiting IRS spectrum very similar to that of EX Lup, were
interpreted by Furlan et al. (2006)
as indicating for the opening of an inner gap in the disk. This might
also give an explanation in case of EX Lup for the lower 6
m
flux compared to that at longer wavelengths. Other sources from their
sample that resemble EX Lup are UY Aur, CZ Tau, and
HP Tau. It is interesting to note that all four objects are binary
systems with different separations.
Finally we calculated the
bolometric temperature and
bolometric luminosity of EX Lup following the method of Chen
et al. (1995). They studied the Taurus and Ophiuchus star-forming
regions, and analyzed the distribution of young stars of different
evolutionary stages in the
vs.
diagram. In a later paper (Chen et al. 1997), they repeated the
study for the objects of the Lupus cloud as well, including EX Lup.
They found
K and
based on IRAS data. Using our newly constructed SED, we recalculated these two values. Assuming AV=0 mag, our result is
K and
L
.
According to these parameters, EX Lup seems to be a typical
classical T Tauri star. The location of EX Lup on the
vs.
diagram implies that it is a Class II object, and its age is
yr.
4.2 Mineralogy
Based on the previous results that EX Lup is similar to classical
T Tauri stars, in the following we assume that its circumstellar
matter is distributed in a disk. To derive the dust composition in the
surface layer of the disk, we fitted the Spitzer IRS spectrum using the
Two-Layer Temperature Distribution
(TLTD) method (Juhász et al. 2009). This method assumes
multicomponent continuum (star, inner rim, disk midplane) and a
distribution of temperatures to fit the source function. The silicate
emission is expected to arise from the disk atmosphere. The observed
spectrum is computed as
where
Here, d is the distance,


Table 4:
Overview of dust species used in fitting the 5-17 m spectrum*.
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Figure 4: Fit of the observed spectrum. The spectral decomposition shows that the mid-infrared spectrum of EX Lup can be reproduced by a mixture of amorphous silicates with olivine and pyroxene stoichiometry. The contribution of crystalline silicates derived from the spectral decomposition is below 2%. |
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In Fig. 4 we present the fit to the 5-17 m
region of the Spitzer IRS spectrum. The derived dust mass fractions are
given in Table 5. The spectral decomposition shows that the main
contributors to the optically thin 10
m silicate emission complex are the amorphous silicates (
in terms of mass). The mass fraction of crystalline silicates is below 2%, which agrees with the value for the diffuse ISM (Kemper et al. 2005). It is interesting to note that the mass-weighted average grain size of the amorphous silicates (0.57
m) in our fit is somewhat larger than typically found in the ISM. At wavelengths longer than 17
m, the IRS spectrum of EX Lup only shows the 18
m feature of the amorphous silicates, and no crystalline feature can be seen.
The fitted values for
,
,
and
are
K,
K, and
K, respectively.
The fitted values for
,
,
and
are
,
,
and
,
respectively.
Although the
of the fit is 14.5, which is far higher than unity, as expected for a good fit, the average deviation from the observed
spectrum is about 1%. The reason for the high
can be found in the relatively high signal-to-noise ratio of the
Spitzer IRS spectrum (>300 in the fitted wavelength range) and in
the deficiencies of the applied dust model (optical constants and
grain-shape model). The latter is probably responsible for the
differences between the 2D RT model and the observed IRS spectrum
between 14 and 21
m.
Given that EX Lup is a young eruptive star, one would expect to
observe an increased value for crystallinity in the mid-infrared
features, compared to ``normal'' T Tauri stars. Since the only
requirement of the crystallization is the high temperature, the
enhanced irradiation luminosity and viscous heating during the
outbursts should lead to rapid crystallization in the disk. In
accordance with our results, Quanz et al. (2007) report the lack of crystalline emission and the presence of emission from larger grains (a>0.1 m)
in the mid-infrared spectra of FU Orionis objects. They hypothesize
that the reason for the lack of crystals can be twofold. One can be the
replenishment of the dust content of the disk atmosphere (where the
mid-infrared features originate) by pristine dust from an infalling
envelope of the FU Ori object. Another possible explanation is strong
vertical mixing in the disk that transports the crystals into deeper
layers of the disk where they cannot be detected
any longer by mid-infrared spectroscopy. Out of these two speculative
scenarios, the latter is favorable for EX Lup, since
to our knowledge, there is no infalling envelope around the source.
Table 5: Fitted dust composition to the Spitzer IRS spectrum, with mass fractions larger than 0.1%.
4.3 Modeling
In this section we perform a detailed modeling of the EX Lup system,
to derive the geometry of its circumstellar environment. We fit the
data points presented in Fig. 1, except the mid-infrared domain
where, due to the intrinsic variability and the different quality of
the data, we considered only the Spitzer measurements: the IRAC and IRS
observations form a quasi-simultaneous high quality data set covering
the 3.6-38 m
wavelength range. Moreover, these measurements are close in time to the
recent 2008 eruption and thus document the pre-outburst conditions of
the system.
For the stellar parameters (radius R*, effective temperature T*, and mass M*) we adopted the values used by Gras-Velázquez & Ray (2005). These parameters were fixed during the modeling. (Table 6 lists all input parameters marking differently the fixed and the optimized ones.) For the distance of the star we adopted 155 pc, the mean distance of the Lupus Complex as measured by the Hipparcos (Lombardi et al. 2008). The unknown location of EX Lup within the complex introduces an additional uncertainty of about 30 pc. For the value of extinction we assumed AV=0 mag (Sect. 3.2).
We used the Monte Carlo radiative transfer code RADMC (Dullemond & Dominik 2004) combined with RAYTRACE.
The circumstellar environment is supposed to be axially symmetric, so
we used a two-dimensional geometry in polar coordinates (
).
As mentioned in Sects. 2.1 and 4.1 we had no indication of an
envelope around EX Lupi, thus our system only consists of a
central star and a dusty disk. For the structure of the disk we assume
the density profile as
![\begin{displaymath}\rho_{\rm disk}(r,z) = \frac{\Sigma (r)}{h(r)\sqrt{2\pi}} \exp{\left\{-\frac{1}{2}\left[ \frac{z}{h(r)}\right]^2\right\}},
\end{displaymath}](/articles/aa/full_html/2009/44/aa11641-09/img98.png)
where r and z are the radial and vertical coordinates, respectively, and


where

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Figure 5: Schematic picture of the geometrical structure of the model. The figure is not to scale. |
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The temperature distribution is determined by the heating sources:
the central star, for which we used a Kurucz model atmosphere (Castelli & Kurucz 2003),
and the heated dust grains emitting blackbody radiation. We used a
passive disk and did not consider accretion, due to the low accretion
rate in quiescence (Sect. 3.3). The accretion luminosity is <1%
of the stellar luminosity, thus its contribution is negligible compared
to direct irradiation coming from the central star. After the
calculation of the temperature distribution, the SED of the system is
produced at an inclination angle
with the ray-tracer.
We used the dust composition derived from the fitting of the Spitzer
IRS spectrum (Sect. 4.2), but excluded dust species whose
contribution to the total mass is 1%. This way, the dust model used in RADMC
contained only amorphous silicates of olivine and of pyroxene types
with a mass ratio of 2:1. The size of the dust grains were 0.1
m and 1.5
m
for olivine and pyroxene stoichiometry, respectively. Besides these, we
added 20% amorphous carbon with a grain size of 0.1
m. The mass absorption coefficients of amorphous carbon were calculated using Mie-theory from the optical constants of Preibisch et al. (1993).
We could reasonably fit most of the measured data points by adopting
the geometry described above. In the best model of this type we had to
move the inner radius of the dusty disk out to 0.5 AU,
significantly exceeding the dust sublimation radius (at T=1500 K) of less than 0.1 AU. However, in the 3-8 m wavelength range this model underestimated the measured points (Fig. 6, dotted line). Using smaller values for the inner radius, we could improve the fit of the 3-5
m range, but then it was not possible to reproduce the measured fluxes at longer wavelengths (Fig. 6,
dashed line). Reducing the inner radius below 0.2 AU the model
fluxes even in the near-infrared wavelength range became too high. To
solve this problem, we introduced a rounded inner rim to the disk (see
inset in Fig. 5); thus instead of having a sharp inner edge with a high wall, we decreased the disk height to
at the beginning of the disk and at the same time moved the inner
radius inward. Behind 0.6 AU we left the structure of the disk
unchanged. With this modification we could obtain a fit that is in good
agreement with all infrared observations. Nevertheless, the inner
radius of 0.2 AU used in the best model is still beyond the
sublimation radius.
Our best-fit model is presented in Fig. 6 with a solid line, and the corresponding parameters listed in Table 6.
In the literature we could not find any constraints for the inclination
of the system, and its value is not defined well by the model either.
The disk is definitely seen closer to face-on then edge-on, and we
obtained our best fit using a value of
,
though fits for inclinations between
(face on) and
are very similar. The outer radius of the circumstellar disk is typical
of young systems, while the disk is massive among T Tauri disks.
For the value of the flaring index
gave the best result, which means that the disk only flares very modestly. The scale height is h=12 AU at the outer radius of the disk, which is slightly higher than the typical value for T Tauri disks.
The exponent of the radial surface density profile is p=-1.0.
![]() |
Figure 6: Spectral energy distribution of EX Lup. The solid line shows our best fit model with the rounded inner wall, while the dashed and dotted lines correspond to the best models using a sharp inner edge. The plotted error bars mark the range of observed fluxes at different epochs, also taking the individual measurement uncertainties into account (filled dots correspond to the middle of the range). Error bars on the IRAC points are smaller then the size of the symbols. |
Open with DEXTER |
Table 6: Parameters used in the best-fit model, where those in italics were adopted from the literature and kept fixed during the modeling.
5 Summary and conclusions
We characterized the quiescent disk of EX Lupi and investigated whether it is the structure of the circumstellar environment that makes it an atypical, eruptive young stellar object. Our main findings are the following:
- During quiescent phase there is an indication of an intrinsic variability of less than 25% in the optical-mid-infrared wavelength regime.
- Our new spectra are consistent with the classification of EX Lup as an M type star. Based on the H
and Pa
spectral lines, we derived a very low quiescent accretion rate of
/yr.
- In general the shape of the SED is similar to those of typical T Tau stars, but above 7
m EX Lup is brighter than the Taurus median by a factor of
2.5. The relative flux contribution from shorter and longer wavelengths is a parameter that may distinguish EX Lup from the majority of classical T Tau stars.
- The 10
m silicate feature of EX Lup can be reproduced well by amorphous silicates with olivine and pyroxene stoichiometry, but no crystalline silicates were found.
- A modestly flaring disk model with a total mass of 0.025
and with inner and outer radii of 0.2 and 150 AU, respectively, is able to reproduce the observed SED. The radius of the inner hole is larger than the dust sublimation radius.
- 1.
- Eisner et al. (2007) claim
that low-mass young stars with low accretion luminosities tend to have
inner disk radii larger than the sublimation radius, probably due to
magnetic field effects. Using the relationship in Eisner et al. (2007) and taking 0.2 AU as the magnetospheric inner radius and an accretion rate of
/yr EX Lupi should have a magnetic field strength of 2.3 kG, which is typical of T Tauri stars (Johns-Krull 2007).
- 2.
- Binarity might also be responsible for clearing up regions of the disk. The case of EX Lup binarity has been studied by several authors. Ghez et al. (1997) used high angular resolution techniques to find wide components, and detected no companion of EX Lup between 150-1800 AU separation. Bailey (1998) detected no companion between 1-10 AU. Melo (2003) claims that EX Lup is not a spectroscopic binary, and similarly Herbig (2007) concludes the same based on spectroscopic data measured by the Keck telescope. Guenther et al. (2007) performed an eight-year long radial velocity monitoring program, but they could not detect binarity in the case of EX Lupi either though they only had 3 spectra. Nevertheless, we note that, if the inclination of EX Lupi is indeed close to a face-on geometry, it makes it difficult to detect a binarity.
- 3.
- Inner gaps are characteristic of disks in the transitional phase between the Class II and Class III stages. These transitional disks, unlike EX Lup, exhibit no excess over the photosphere in the near-infrared wavelength range. Furlan et al. (2006) suggest that IRAS 04385+2550, an object whose SED is similar to that of EX Lup, could be in a state preceding the transition. This explanation would mean that EX Lup might also be in a pre-transitional state.
- 4.
- Alternatively, with such a low accretion rate, photoevaporation by EUV radiation may also contribute to the clearing of this innermost region (Gorti & Hollenbach 2009).
- 5.
- It cannot be excluded that the large inner hole is a pheanomenon connected with the eruptive behavior, although details of this connection are unclear yet.
One of our main goals in the present work was to identify atypical features in the circumstellar structure of EX Lup, which may explain its eruptive nature. The inner-disk hole revealed by our modeling is an unexpected result in this sense and comparison of EX Lup with other EXors at infrared wavelengths would be important. It may answer the question of whether an inner gap in the dusty disk is characteristic of the EXor phenomenon connecting the hole to the eruption mechanism, and we could learn to what extent EX Lup is a good representative of eruptive stars.
AcknowledgementsThe work was supported by the grants OTKA T 49082 and OTKA K 62304 of the Hungarian Scientific Research Fund. The authors are grateful to C.P. Dullemond for kindly providing RAYTRACE and also to Jeroen Bouwman for providing his routines for the Spitzer IRS data reduction. The research of Á.K. is supported by the Nederlands Organization for Scientific Research. They also acknowledge for observational data from the AAVSO International Database contributed by observers worldwide.
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Footnotes
- ... quiescence
- Full Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/507/881
- ... Database
- www.aavso.org
- ...
IPAC
- http://scanpiops.ipac.caltech.edu:9000/applications/Scanpi/
- ...RAYTRACE
- For details see: http://www.mpia.de/homes/dullemon/radtrans/radmc/
All Tables
Table 1: Optical and infrared observations of EX Lup collected from the literature, obtained in its quiescent periods.
Table 2: Color-corrected fluxes of EX Lupi*.
Table 3: Observed wavelength, EW, and FWHM of the most prominent emission lines in the optical spectrum of EX Lupi in quiescence*.
Table 4:
Overview of dust species used in fitting the 5-17 m spectrum*.
Table 5: Fitted dust composition to the Spitzer IRS spectrum, with mass fractions larger than 0.1%.
Table 6: Parameters used in the best-fit model, where those in italics were adopted from the literature and kept fixed during the modeling.
All Figures
![]() |
Figure 1:
Spectral energy distribution of EX Lup, showing all data points
from Tables 1 and 2 and the smoothed spectra obtained with
NTT/SOFI, ISOPHOT-S, and Spitzer/IRS. The gray stripe marks the median
SED of T Tauri objects from the Taurus-Auriga star-forming region.
The 5-36 |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Details of the optical spectrum of EX Lupi showing significant or
typical features. The interval shown in the second panel of the upper row is
the same as Herbig's (2007) Fig. 3. It is apparent that the
broad component of the Fe II |
Open with DEXTER | |
In the text |
![]() |
Figure 3: Near-infrared spectrum of EX Lupi, observed on 2001 May 4. The region around the 12CO bandhead absorption is enlarged in the inset. |
Open with DEXTER | |
In the text |
![]() |
Figure 4: Fit of the observed spectrum. The spectral decomposition shows that the mid-infrared spectrum of EX Lup can be reproduced by a mixture of amorphous silicates with olivine and pyroxene stoichiometry. The contribution of crystalline silicates derived from the spectral decomposition is below 2%. |
Open with DEXTER | |
In the text |
![]() |
Figure 5: Schematic picture of the geometrical structure of the model. The figure is not to scale. |
Open with DEXTER | |
In the text |
![]() |
Figure 6: Spectral energy distribution of EX Lup. The solid line shows our best fit model with the rounded inner wall, while the dashed and dotted lines correspond to the best models using a sharp inner edge. The plotted error bars mark the range of observed fluxes at different epochs, also taking the individual measurement uncertainties into account (filled dots correspond to the middle of the range). Error bars on the IRAC points are smaller then the size of the symbols. |
Open with DEXTER | |
In the text |
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