Issue |
A&A
Volume 511, February 2010
|
|
---|---|---|
Article Number | L7 | |
Number of page(s) | 4 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/200913832 | |
Published online | 10 March 2010 |
LETTER TO THE EDITOR
HR 7355 - another rapidly braking He-strong CP star?![[*]](/icons/foot_motif.png)
Z. Mikulásek1,5 - J. Krticka1 - G. W. Henry2 - S. N. de Villiers3 - E. Paunzen4 - M. Zejda1
1 - Department of Theoretical Physics and Astrophysics,
Masaryk University, Brno, Czech Republic
2 -
Center of Excellence in Information Systems, Tennessee
State University, Nashville, Tennessee, USA
3 -
Private Observatory, 61 Dick Burton Road, Plumstead,
Cape Town, South Africa
4 -
Institute for Astronomy of the University of Vienna,
Vienna, Austria
5 -
Observatory and Planetarium of J. Palisa, VSB -
Technical University, Ostrava, Czech Republic
Received 9 December 2009 / Accepted 4 February 2010
Abstract
Context. Strong meridional mixing induced by rapid rotation
is one reason why all hot main-sequence stars are not chemically
peculiar. However, the finding that the He-strong CP star HR 7355
is a rapid rotator complicates this concept.
Aims. Our goal is to explain the observed behaviour of HR 7355 based on period analysis of all available photometry.
Methods. Over two years, we acquired 114 new BV
observations of HR 7355 at observatories in Arizona,
U.S.A and Cape Town, South Africa. We performed period analyses of the
new observations along with new analyses of 732 archival measurements
from the Hipparcos and ASAS projects.
Results. We find that the light curves of HR 7355
in various filters are quite similar, with amplitudes 0.035(4),
0.036(4), and 0.038(3) mag in B, Hp, and V,
respectively. The light curves are double-peaked, with unevenly deep
minima. We substantially refine the rotational period to be
,
indicating that HR 7355 is the most rapidly rotating CP
star known. Our period analyses reveal a possible lengthening of the
rotational period with
.
Conclusions. We conclude that the shape and amplitude of
HR 7355 light curves are typical of magnetic He-strong
CP stars, for which light variations are the result of photospheric
spots on the surface of a rotating star. We hypothesise that the light
variations are caused mainly by an uneven distribution of overabundant
helium on the star's surface. We briefly describe and discuss the cause
of the rapid rotational braking of the star.
Key words: stars: chemically peculiar - stars: variables: general - stars: individual: HR 7355 - stars: rotation
1 Introduction
Chemically peculiar (CP) stars are an important class of stars that occupy the upper main sequence, where radiative diffusion and gravitational settling result in atmospheric chemical abundances that differ remarkably from the Sun's. According to their patterns of chemical anomalies, CP stars are classified into several subclasses that also follow a temperature sequence. Among them, SrCrEu, Si, He-weak, and He-strong stars have strong global magnetic fields. These ``magnetic'' CP (mCP) stars also exhibit synchronous variability in their spectra and brightness with periods longer than one half of a day. Their photometric amplitudes are a few hundredths of magnitude.
mCP stars have inhomogeneous surface distributions of chemical elements as determined from their rotationally modulated spectral-line variability (e.g., Lüftinger et al. 2010b,a). The uneven surface distribution of various elements, together with rotation, has been presumed to be the main cause of these stars' light variability. Line blanketing caused by overabundant elements, mainly iron-group metals and b-f transitions, may induce the flux redistribution providing the mechanism for the light variability (Lanz et al. 1996). A strong magnetic field may also influence the light curves (e.g., Kochukhov et al. 2005).
Krticka et al. (2007,2009) used surface abundance maps to simulate successfully the light curves of the He-strong star HD 37776 and the Si star HR 7224. They demonstrated that the inhomogeneous surface distribution of silicon, iron, and helium, along with the b-f and b-b transitions of these elements, accounted for most of the light variability in these CP stars.
The light curves of magnetic CP stars are stable on a timescale of decades or more and so indicate persistency of their spectroscopic and photometric spots. We can observe period changes in their light curves in only a few cases (Mikulásek et al. 2008b, and references therein).
It is generally expected that the meridional currents induced by the rapid rotation of hot MS stars are able to erase the effects of the slow diffusion of chemical elements and thus prevent the formation of CP abundance anomalies. We study therefore the light variability of HR 7355, which is one of the most rapidly rotating mCP stars.
2 The star
HR 7355 (HD 182180, HIP 95480) is a bright (V=6.02 mag) but
poorly studied southern B2V star. It is known to be a rapid rotator,
Oksala et al. (2010) evaluating its projected equatorial velocity to be
.
The Hipparcos catalog
(ESA 1997) classified the star as an ``unsolved variable'', but
Koen & Eyer (2002) reanalysed the Hipparcos photometry and found a
frequency of variation of
.
The first detailed study of HR 7355 was performed by Rivinius et al. (2008),
who describe the star as a helium-strong CP star with Balmer
emission. They argue that the true period, corresponding to the
star's rotational period, is twice that derived by Koen & Eyer (2002):
.
This suggests that HR 7355 is the most rapidly
rotating He-strong CP star known.
In the present study, we analyse our new and archival photometry of HR 7355 to determine the star's periodicity and light curve shape at various epochs between 1990 and 2009.
2.1 Parameters of the star
We estimate the mass and age of HR 7355 using the revised version
of the Hipparcos catalogue (van Leeuwen 2007), the Geneva and
Strömgren photometry (from
GCPD), and the isochrones
of the Padova group (Marigo et al. 2008).
The Geneva colours (Cramer 1999) are consistent with a B2 V star. The Z index shows no peculiarity beyond what we would expect for a classical CP4 star (Paunzen et al. 2005). From the various Geneva indices and the available Strömgren photometry, we deduce a reddening of E(b-y) = 0.05 mag and an effective temperature of 18 000 K. The photometric estimates for the absolute magnitude, MV, vary between -1.75 and -1.95 mag. The parallax gives a distance of 273(26) pc and an absolute magnitude of MV=-1.38(0.20) mag (assuming V = 6.02 mag). This result is fainter than those estimated from the photometric indices, which may be a result of the star's rapid rotation.
We estimate the age of HR 7355 to be between 15 and 25 Myr, as
derived from the parallax-based and the photometry-based values of
MV, respectively. We note that Westin (1985) lists
(23.9 Myr) for HR 7355. Consequently, HR 7355 appears to
be near the middle of its main-sequence lifetime. We derive a mass
of 6.3(0.3)
from the parallax-based MV. The
photometry-based absolute magnitude would result in a higher mass.
From its distance and the Galactic coordinates, we derive the Galactic [X,Y] distances/coordinates of HR 7355 to be [+254,+48] pc. Comparing these values and their uncertainties with the borders of the Scorpius-Centaurus association (Preibisch & Mamajek 2008), we find that HR 7355 is probably beyond the outer edge of the association. The mean proper motion of the association is [-25,-10] mas yr-1 (de Zeeuw et al. 1999), compared to [+12,-15] mas yr-1 for HR 7355. Given its motion direction and apparent age, we suggest that HR 7355 does not originate in the Scorpius-Centaurus association.
3 Photometric data of HR 7355
3.1 New photometry
Most of our new photometry of HR 7355 was acquired with the T3
0.4 m automatic photoelectric telescope (APT) at Fairborn
Observatory in southern Arizona during 2008 May and June. The T3 APT
uses a temperature-stabilised EMI 9924B photomultiplier tube to
measure photon count rates sequentially through B and V filters.
For additional details about the collection and reduction of the APT
data, see cf. Mikulásek et al. (2008b) and references therein. The comparison
and check star used by the APT were HD 179520 and HD 181240,
respectively. The southern declination of HR 7355 (
)
causes airmass values of
2 for all of
our APT measurements. The standard deviation of the difference
between variable and comparison stars is
0.01 mag, twice the
typical scatter with this telescope. Thus we acquired 43 B and 38 V measurements.
We also obtained seven continuous hours of BV photometry with a photoelectric photometer attached to a 0.28 m reflector on the night of 2009 July 26 UT at the private observatory of one of us (SNdV) in Cape Town, South Africa. We acquired 17 and 16 measurements in Vand B. The comparison and check stars were the same as used by the APT; the scatter in the observations was 0.01 mag. When combined with the APT measurements, these continuous single-night observations helped us to minimise the aliasing inherent in single-sight data sets.
The newly acquired photometric data are available at the CDS or
the On-line database of photometric observations of mCP
stars
.
3.2 Archival photometry
The Hipparcos photometry (ESA 1997) of HR 7355 consists of 57 measurements in
(scatter
of 23 mmag), 45
in Hp (
mmag), and 56 in
(
mmag). The data cover the period from 1990 March to 1993 March.
The continuously updated archive of the All Sky Automated Survey (ASAS) (Pojmanski 2002) is a useful source of photometric observations of stars near the equator. Unfortunately, the precision for relatively bright stars is poor - the data have significant non-Gaussian scatter with plenty of outliers. Furthermore, the data contain a long-term trend with a range of 0.05 mag.
Nonetheless, the ASAS data are the only photometric data of HR 7355 available in the period between the end of the Hipparcos mission (1993) and the start of our own photometry (2008). We extracted only the individual V measurements with a quality of ``A'' or ``B'' and removed the long-term trend. This resulted in an ASAS data set of 574 V observations covering the time interval from 2001 February to 2009 October. These data have a scatter of 50 mmag.
Therefore, we consider in our period analysis a total of 846 measurements spread over 20 years.
4 The ephemeris
4.1 The period
The periodogram of all available HR 7355 photometry displays only
two prominent peaks - one at a period of
and the second
at
- that agree well with the previous determinations
of Koen & Eyer (2002) and Rivinius et al. (2008). The shorter period is the
consequence of the double-peaked nature of the light curve (see Fig. 1). This
period is shorter than the critical
period of centrifugal disruption of main-sequence stars of the same
spectral type and so cannot represent HR 7355's rotation period,
which we take to be
.
The longer period is also
compatible with the period of the well documented spectral and
spectropolarimetric variations (Rivinius et al. 2010; Oksala et al. 2010).
![]() |
Figure 1:
BHpV light curves plotted versus the quadratic
phase. |
Open with DEXTER |
4.2 The light variations model
The double-waved light curves in B, Hp, and V are
similar (see Fig. 1), differing only slightly in their
effective amplitudes Ac (for the definition see Mikulásek et al. 2007),
where the subscript c denotes the filter colour. Light-curve
magnitudes can then be expressed as
where mcj(t) is the magnitude in colour c observed by j-th observer,






where

where M01 is the maximum nearest the weighted center of the observations, P1 is the period of the linear fit,





All 19 model parameters were computed simultaneously by a weighted non-linear LSM regression applied to the complete observational material without any artificial divisions.
![]() |
Figure 2:
Time variation in mutual phase shifts of observed light
curves in days computed with a linear ephemeris. |
Open with DEXTER |
4.3 Results
We determined the model parameters
,
s y-1, and
.
Time of the
primary maximum being given by
where E is an integer. The effective amplitudes Ac are almost identical and equal to 0.035(4), 0.036(4), and 0.038(3) mag in B, Hp, and V, respectively,


The reliability of the LSM procedure results depends critically on the appropriateness of the chosen model for the description of the reality - in our case light variations over the past twenty years. Inspecting Fig. 1, we can conclude that the model of light curves described by Eqs. (1) and (2) is fully adequate.
Adequacy of the quadratic model used for the phase function
Eq. (3) can be tested by changes in mutual phase shifts
of observed light curves. The shift (O-C)k can be evaluated for
any subset k of observational data by the relation:
(O-C)
,
where
are deviations of observed magnitudes from the fit, and
are time derivatives of the fitted function
(Mikulásek et al. 2006). From Fig. 2 containing shifts of 6
observational data subsets with respect to the linear ephemeris, we
conclude that our quadratic model of the phase function in
Eq. (3) is acceptable.
To be sure that non-zero
is not a mere conjunction of the
non-Gaussian noise in ASAS data, we treated the observational set
excluding all the ASAS data. Even in this case, we obtained
,
supporting the reality of the period
lengthening.
5 Discussion
5.1 HR 7355 - the most rapidly rotating CP star
The
rotational period of HR 7355 is among the
shortest known to date for CP stars: HD 164429
(
,
Adelman 1999); HD 124224 = CU Vir
(
,
Sokolov 2000); HD 92385
(
,
ESA 1997). Among these fast rotating CP stars,
HR 7355 is the hottest, most massive and, consequently, the largest
thus, we conclude that HR 7355 has the largest equatorial
rotational velocity (
using the parallax-based MV for a B2 V star and
the period) and also the highest ratio of equatorial velocity to
critical equatorial velocity
among all known CP
stars. Therefore, we consider HR 7355 to be the most rapid rotator
of all known chemically peculiar stars. Because of its rapid
rotation, it can serve as an important benchmark for theories
describing the influence of rotational mixing on chemical
peculiarity.
5.2 Nature of the light variation
Our analysis of the B, Hp, and V light curves demonstrates that all three passbands have the same effective amplitude. This suggests that the variability mechanism at optical wavelengths could be unique (Mikulásek et al. 2008a). We suggest that these light variations are caused by the uneven distribution of optically active, overabundant elements on the surface of the star. Unfortunately, we do not have maps of the abundance distribution or spectrograms suitable for their creation.
We consider the possibility that the broad-band optical light
variability in HR 7355 arises from variations in the spectral lines
of
,
,
and
,
as depicted
for HR 7355 in Fig. 1 of Rivinius et al. (2008). They compare the line
profiles of two spectra obtained at quadrature (HJD
and HJD
,
as defined for
Eq. (3)); their first spectrum was thus taken shortly
after secondary light maximum, while the second was acquired at the
secondary light minimum. The only overabundant element whose line
intensity reaches maximum in the optical is helium (see the
relevant analysis of He-strong HD 37776 in Krticka et al. 2007). Lines of the
other ions mentioned above are relatively weak and nearly constant.
The photometric effect of the weak emission in H
is also
negligible.
We modelled the light curves of HR 7355 with the code described by
Krticka et al. (2007) assuming the inclination angle of
(
km s-1, Oksala et al. 2010) and found that two circular, helium-rich spots
with [He/H]=1.4 and radii
on opposite hemispheres of
HR 7355 reproduce the observed light variations in all
three
passbands. We therefore conclude that light variations in
HR 7355 may be the result of the uneven distribution of
helium.
This hypothesis should be tested with Doppler tomography, which we plan to do in the near future.
5.3 Rotational braking and its nature
An increase in the rotational period with
is observed at the
level
of certainty. During the past 20 years, the period has increased
by 2.1 s! Unfortunately, no observations were taken in the
interval 1994-2000. This adds some uncertainty to our quadratic
fit of the
O-C residuals. If the period change were real, then
HR 7355 would
be the fourth known CP star displaying an increase in its rotational
period.
The star is similar in several aspects to the most rapidly braking
He-strong CP star HD 37776 with a well-determined
year-1(Mikulásek et al. 2008b). The period increase in HR 7355 could also be
interpreted as a deceleration of the rotation of its surface
layers due to momentum loss by a magnetically confined stellar wind
(see also ud-Doula et al. 2009). However, a possible change in the rate of
period change for HD 37776
(
d-1) suggests that the
process of the rotational braking need not be fully monotonic!
Both stars have strong magnetic fields; that of HR 7355 is
approximately dipolar ranging in strength from -2 kG to +2.5 kG
(Oksala et al. 2010), while the field of HD 37776 is dominated by a
quadruple component (Thompson & Landstreet 1985).However, the main difference
between the stars discussed here is their age. While HD 37776 is a
very young CP star with an age of around 1 Myr, HR 7355 is about
twenty times older (see Sect. 2.1). Because the characteristic
braking time of HR 7355 (
yr) is
about fifty times shorter than its stellar age, it seems probable
that variations in rotational period are confined to the outer
layers of the star. The period variations could be cyclic with a
long interval of period increase followed by a rapid period
decrease. The period decrease may be caused by greater friction
between the surface and inner layers of the star caused by, e.g.,
reconnection events. The length of this cycle can be roughly
estimated as the time when the surface layers lag behind the inner
part of the star by one revolution (i.e.,
). This produces estimates of 35 yr and 45 yr
for HR 7355 and HD 37776, respectively. The hypothesis should be
tested a few decades hence with additional observations.
6 Conclusions
We have improved the accuracy of the rotational period of the most
rapidly rotating CP star HR 7355 to
and
determined its rate of period change to be
.
We propose that the period variations
could be cyclic on a timescale of a few decades. Observed light
variations may be caused by the uneven surface distribution of
overabundant helium. HR 7355 remains a very appealing target for
continued photometric and spectroscopic observations, as well as for
the modelling of its unusual behaviour.
Supports of grants GAAV IAA301630901 and MEB 060807/WTZ CZ-11/2008 are acknowledged. G.W.H. acknowledges long-term support from NASA, NSF, Tennessee State University, and the state of Tennessee through its Centers of Excellence program. E.P. acknowledges support by the City of Vienna (Hochschuljubiläumsstiftung project: H-1930/2008). We thank to dr. D. A. Bohlender for his inspiring refereeing of the article.
References
- Adelman, S. 1999, A&AS, 136, 379 [Google Scholar]
- Cramer, N. 1999, New Astron., 43, 343 [NASA ADS] [CrossRef] [Google Scholar]
- de Zeeuw, P. T., Hoogerwerf, R., & de Bruijne, J. H. J., et al. 1999, AJ, 117, 354 [NASA ADS] [CrossRef] [Google Scholar]
- ESA 1997, in The Hipparcos and Tycho Catalogues, ESA SP-1200, Noordwijk [Google Scholar]
- Koen, C., & Eyer, L. 2002, MNRAS, 331, 45 [NASA ADS] [CrossRef] [Google Scholar]
- Kochukhov, O., Khan, S., & Shulyak, D. 2005, A&A, 433, 671 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Krticka, J., Mikulásek, Z., Zverko, J., & Ziznovský, J. 2007, A&A, 470, 1089 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Krticka, J., Mikulásek, Z., Henry, G. W., et al. 2009 A&A, 499, 567 [Google Scholar]
- Lanz, T., Artru, M.-C., Le Dourneuf, M., & Hubeny, I. 1996, A&A, 309, 218 [NASA ADS] [Google Scholar]
- Lüftinger, T., Fröhlich, H.-E., Weiss, W. W., et al. 2010a, A&A, 509, A43 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Lüftinger, T., Kochukov, O., Ryabchikova, T., et al. 2010b, A&A, 509, A71 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Marigo, P., Girardi, L., Bressan, A., et al. 2008, A&A, 482, 883 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Mikulásek, Z., Wolf, M., Zejda, M., & Pecharová, P. 2006, Ap&SS, 304, 363 [NASA ADS] [CrossRef] [Google Scholar]
- Mikulásek, Z., Janík, J. Zverko, J., et al. 2007, Astron. Nachr., 328, 10 [NASA ADS] [CrossRef] [Google Scholar]
- Mikulásek, Z., Gráf, T., Krticka, J., Zverko, J., & Ziznovský, J. 2008a, Contrib. Astron. Obs. Sk. Pleso, 38, 363 [NASA ADS] [Google Scholar]
- Mikulásek, Z., Krticka, J., Henry, G. W., et al. 2008b, A&A, 485, 585 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Oksala, M., Wade, G., Wagner, M., et al. 2010, MNRAS, submitted [Google Scholar]
- Paunzen, E., Stütz, Ch., & Maitzen, H. M. 2005, A&A, 441, 631 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Pojmanski, G. 2002, , 52, 397 [Google Scholar]
- Preibisch, T., & Mamajek, E. 2008, Handbook of Star Forming Regions, Vol. II: The Southern Sky ASP Monograph Publications, ed. Bo Reipurth, 5, 235 [Google Scholar]
- Rivinius, T., Stefl, S., Townsend, R. H. D., & Baade, D. 2008, A&A, 482, 255 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Rivinius, T., Szeifert, T., Barrera, L., et al. 2010, MNRAS, submitted [Google Scholar]
- Sokolov, N. A. 2000, A&A, 353, 707 [NASA ADS] [Google Scholar]
- ud-Doula, A., Owocki, S. P., & Townsend, R. H. D. 2009, MNRAS, 392, 1022 [NASA ADS] [CrossRef] [Google Scholar]
- Thompson, I. B., & Landstreet, J. D. 1985, ApJ, 289, L9 [NASA ADS] [CrossRef] [Google Scholar]
- van Leeuwen, F. 2007, A&A, 474, 653 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Westin, T. N. G. 1985, A&AS, 60, 99 [Google Scholar]
Footnotes
- ... star?
- Photometric data are 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/511/L7
- ...
GCPD
- http://obswww.unige.ch/gcpd
- ... CDS
- http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/511/L7
- ...
stars
- http://astro.physics.muni.cz/mcpod
All Figures
![]() |
Figure 1:
BHpV light curves plotted versus the quadratic
phase. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Time variation in mutual phase shifts of observed light
curves in days computed with a linear ephemeris. |
Open with DEXTER | |
In the text |
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