Study of the Long-term BVRcIc Photometric Variability of Eight PMS Stars in the Young Open Cluster Trumpler 37*

Sunay Ibryamov ,Gabriela Zidarova ,Evgeni Semkov ,and Stoyanka Peneva

1 Department of Physics and Astronomy,Faculty of Natural Sciences,University of Shumen,115,Universitetska Str.,9700 Shumen,Bulgaria;sibryamov@shu.bg

2 Institute of Astronomy and National Astronomical Observatory,Bulgarian Academy of Sciences,72,Tsarigradsko Shose Blvd.,1784 Sofia,Bulgaria

Abstract This paper reports results from our long-term BV(RI)c photometric CCD observations of eight pre-main sequence stars collected from 2008 June to 2022 October.These stars are located in the young open cluster Trumpler 37,in the field of GM Cephei.The observational data indicate that all stars from our study exhibit variability in all-optical passbands,typical for young stars.In this paper,we describe and discuss the photometric behavior of the stars and the possible reasons for their variability.For two of the objects,we identified periodicity in their light variation.

Key words: stars: pre-main sequence– stars: variables: T Tauri– Herbig Ae/Be

1.Introduction

Trumpler 37 is a young open cluster and it is immersed in the H II region IC 1396.This cluster was identified with the nucleus of the Cepheus OB2 association (Simonson 1968).Patel et al.(1995)suggested that the stars forming in the globules of IC 1396 represent the youngest generation of stars in the Cepheus region.Marschall et al.(1990) obtained photoelectricUBVobservations of 120 stars in Trumpler 37 and derived its age of 6.7 Myr.The authors also established that the cluster contains many possible pre-main sequence (PMS) stars.The latest age estimation of Trumpler 37 yields ∼4 Myr (Sicilia-Aguilar et al.2005) and the distance determined to it by Contreras et al.(2002)is 870 pc.The cluster was an object of many studies,the recent of which were published by Sicilia-Aguilar et al.(2005,2006,2010),Barentsen et al.(2011),Meng et al.(2019),etc.

PMS stars are young stars in the early stages of stellar evolution.They are divided into two main groups,which are T Tauri stars(TTSs)with relatively low mass(M≤2M⊙)and the more massive (2M⊙≤M≤8M⊙) Herbig Ae/Be (HAEBE)stars.One of the main features of both groups of PMS stars is their photometric variability.

The study of TTSs began in the middle of the 20th century by Joy(1945).TTSs are separated into two subgroups −classical T Tauri stars (CTTSs) and weak-line T Tauri stars (WTTSs).The CTTSs are surrounded by spacious accreting circumstellar disks,whereas they must have almost disappeared (at least their inner parts) in the WTTSs (Ménard &Bertout 1999).The presence or absence of an active accretion disk determines most of the features that characterize each subgroup of TTSs.Reviews of the characteristics of TTSs were given in the works of Cram &Kuhi (1989) and Petrov (2003).

A detailed study of the various causes of the variability of TTSs was carried out by Herbst et al.(1994),based on a large electronicUBVRIcatalog that includes several hundred stars.According to Herbst et al.(1994),the variability of WTTSs is due to cool spots on the stellar surface.The periods of this variability are observed on timescales of days and with amplitudes up to 0.8 mag(V)and 0.5 mag (I).WTTSs can also show flares related to surface magnetic activity.The causes of the variability of CTTSs are more complicated.These stars exhibit irregular brightness variations on timescales of hours and with amplitudes up to 2.6 mag (V) and 1.6 mag(I).The variations in mass accretion rate and the presence of hot and cool (in some CTTSs) spots on the stellar surface are responsible for the variability of the CTTSs.

In some young stars large amplitude dips in their brightness can be observed.These objects are called UXors,named after their prototype UX Orionis.The UXors generally exhibit irregular variations on timescales of days to weeks and with amplitudes up to 2.8 mag.It is generally accepted that the registered minima in the brightness of these objects result from the variable circumstellar obscuration (Zaitseva 1986;Voshchinnikov 1989;Grinin et al.1991;Herbst et al.1994).During the deep minima,the UXors often become bluer as they fade.This is the so-called blueing effect or color reverse(see Bibo&Thé 1990).The reason for this effect is that when the circumstellar clouds of dust and gas or cometary bodies,orbiting the central star,cross the line of sight,a decrease in the brightness of the star occurs.Initially,the star becomes redder,but during a large extinction the scattered light from the dust clumps begins to dominate and the star becomes bluer.In the work of Dullemond et al.(2003) the UXors’variability was explained with self-shadowed disks.

In this study,we present results from theBV(RI)cphotometric monitoring of eight stars,located in the cluster Trumpler 37,in the field of GM Cep.On the basis of the longterm light curves of the stars,we discuss their photometric behavior and the probable causes of their variability.Our studies of the star GM Cep itself were published in Semkov&Peneva(2012),Semkov et al.(2015)and Mutafov et al.(2022).In Section 2 of this paper,we give information about the telescopes and CCD cameras used and the process of data reduction.In Section 3 we describe the results obtained for the investigated stars and their interpretation.Finally,in Section 4 we briefly present the concluding remarks.

2.Observations and Data Reduction

Our observations of the field centered on GM Cep were obtained during the period from 2008 June to 2022 October with four telescopes and six different CCD cameras as follows −the 2 m Ritchey-Chrétien-Coudé (with cameras VersArray 1300B and Andor iKon-L),the 50/70 cm Schmidt(with cameras SBIG STL-11000M and FLI PL16803)and the 60 cm Cassegrain(with camera FLI PL09000) telescopes of the Rozhen National Astronomical Observatory in Bulgaria and the 1.3 m Ritchey-Chrétien (with camera Andor DZ436-BV)telescope of the Skinakas Observatory3Skinakas Observatory is a collaborative project of the University of Crete,the Foundation for Research and Technology,Greece,and the Max-Planck-Institut für Extraterrestrische Physik,Germany.of the University of Crete in Greece.The observational procedure and technical parameters of the CCD cameras used are given in Ibryamov et al.(2015)and Ibryamov&Semkov(2020).

All frames were obtained through a standard Johnson−Cousins(BVRcIc)set of filters.The observational data were reduced by applying standard IDL procedures,adapted from DAOPHOT.As a reference,the comparison sequence reported in Semkov &Peneva (2012) was used.All data were analyzed using the same aperture,which was chosen to have a 6〞 radius,while the background annulus was taken from 10〞 to 15〞.The mean value of errors in the reported magnitudes is 0.01–0.03 mag for theIcandRcband data,0.01–0.04 mag for theVband data,and 0.01–0.05 mag for theBband data.

3.Results and Discussion

We listed the stars from our study in Table 1.The table columns contain the 2MASS designations,equatorial coordinates and the number of photometric points obtained for each star with different telescopes used.Because of the different fields of view of the telescopes and cameras used,we have a different number of photometric points for each star.Figure 1 shows a three-color image of the field,where the positions of the stars from our study and GM Cep are marked.

Table 1Designations,Equatorial Coordinates and Number of Observations of the Stars

Table 2 presents a small fraction of the photometric CCD observations of 2MASS J21382596+5734093 as a guideline on the form and content of the full tables for each star.The table columns contain Date (dd.mm.yyyy format) and Julian date (JD) of the observation,the measured magnitudes of the star,and the telescope and CCD camera employed.

Table 2Photometric CCD Observations of 2MASS J21382596+5734093

In Table 3 we report theBV(RI)cmaximal and minimal magnitudes and the amplitudes of the variability of the investigated stars registered during our monitoring.It can be seen from Table 3 that the lowest amplitude star is 2MASS J21365072+5731106 (ΔV=0.14 mag),theVamplitude of six stars is in the range from 0.56 to 1.54 and the largest amplitude star is 2MASS J21393480+5723277 (ΔV=2.03 mag).The stellar parameters of the objects from the literature are summarized in Table 4.

Table 3The Registered BV(RI)c Maximal and Minimal Magnitudes and the Amplitudes of the Variability of the Stars

Table 4Stellar Parameters of the Stars

We used the PERIOD04 (Lenz &Breger 2005) and PERSEA(written by G.Maciejewski,based on Schwarzenberg-Czerny 1996) software packages to search for periodicity in the photometric variability of the objects.We discuss the obtained photometric results for the stars in the following subsections.

3.1.2MASS J21365072+5731106(Also Known as LkHα 349,HBC 308 and V390 Cep)

LkHα 349 is a central nebulous star of the nebula IC 1396A and it lies at the focus of a large parabolic rim of emission nebulosity in IC 1396(see Loren et al.1975 and Nakano et al.1989).This star was included in the work of Dibai &Esipov (1968),where the authors presented its spectrum.According to the authors,LkHα 349 exhibits a strong continuous spectrum with sharply defined emission in the Hα line and they reported the mean measurements from the photoelectric observations (from 1966 July) of the star:B=15.25 mag andV=13.40 mag.Dibai &Esipov (1968) also noted that the star is very red and that probably most of the reddening is due to the absorption of light in the dense globule.They are unable to determine the intrinsic color of the star(its spectral type) because of the lack of lines.

LkHα 349 was included in the Second Catalog of Emission-Line Stars of the Orion Population published by Herbig &Kameswara Rao (1972).Cohen &Kuhi (1979) determined its spectrum as F8 and reported that it has a striking P Cygni profile at Hα.

Hessman et al.(1995) conducted a detailed study of LkHα 349 and concluded that it is a PMS star of intermediate mass(≥3M⊙) on its way to becoming a Herbig Be star.Hessman et al.(1995) presented a historical photographicBlight curve of the star for the period from 1899 to ∼1990,obtained from the measurements on plates in the different plate archives.For this period of time the star’sBbrightness varies in the range from 13 to 16.2 mag.Based on the historical light curve,Kazarovets &Samus (1997) cataloged LkHα 349 in the 73rdName-List of Variable Stars with the designation V390 Cep.

Marschall et al.(1990) measuredV=13.41 mag,B−V=1.71 mag,V−R=1.06 mag andR−I=1.07 mag for LkHα 349.Fernandez (1995) presented 27BV(RIc) photometric points of the star,obtained in the period from 1991 August to 1992 August.In the presented analysis of these data in Fernandez &Eiroa (1996),the authors concluded that the star’s brightness is constant during the observations until the last nights in 1992 August,when it decreased 0.1 mag in all bands.According to their data,the mean value of the star’sVbrightness is 13.37 mag.

TheBV(RI)clight curves of LkHα 349 from our observations(the circles) are plotted in Figure 2.For this star,we found photometric data in the database of the American Association of Variable Star Observers (AAVSO,https://www.aavso.org/)and included them in the figure(the empty diamonds).It is seen that there is a good match between our data and ones from AAVSO.The available data on LkHα 349 suggest that it exhibits variability with small amplitudes.As can be seen from Figure 2 and Table 3,the registered amplitude of the star’s light variation is under 0.2 mag in all optical passbands.Variability with such small amplitudes is typical for both WTTSs and HAEBEs,and it likely is produced by cool spots on the star’s surface.

Figure 2. BVRcIc light curves of 2MASS J21365072+5731106.The circles represent our data and the empty diamonds signify the data from AAVSO.

Using our data and ones from AAVSO,we carried out a periodicity search in the photometric behavior of LkHα 349.Initially,we used all data obtained during the whole time of the observations,and then the data only from different periods.However,we did not detect any periodicity in the star’s variability.

3.2.2MASS J21381703+5739265 and 2MASS J21403574+5734550

The light curves of 2MASS J21381703+5739265 and 2MASS J21403574+5734550 from ourBV(RI)cmonitoring are displayed in Figures 3 and 4,respectively.The data indicate that the photometric behavior of both stars is characterized by strong irregular variability in all-optical passbands.

It is seen from Figure 3 that the total brightness of 2MASS J21381703+5739265 gradually decreases until mid-2014,then it begins to increase and reaches its previous high level toward the end of 2018.Then,the star’s total brightness begins to decrease again.During our observations,several single dips in the variability of the star are also registered.

Figure 3. BVRcIc light curves (left) and color−magnitude diagrams (right) of 2MASS J21381703+5739265.

The amplitudes of the light variations of 2MASS J21381703+5739265 are given in Table 3.Usually,such amplitudes are typical of CTTSs surrounded by a circumstellar disk.The star’s color variations versus theVmagnitude (Figure 3) are typical for TTSs.The possible reasons for the variability of 2MASS J21381703+5739265 can be different,which include a change in mass accretion rate from the circumstellar disk and the presence of spot(s) on the star’s surface.

For 2MASS J21403574+5734550 our data suggest that its brightness generally varies around some intermediate level.It can be seen from the color−magnitude diagrams for the star(Figure 4) that it becomes redder as it fades,typical for TTSs.The registered amplitudes for the star’s variability are given in Table 3.It can be assumed that variability with such properties is typical of both subgroups of TTSs and it probably is produced by the rotational modulation of spot(s) on the star’s surface.

Figure 4. BVRcIc light curves (left) and color−magnitude diagrams (right) of 2MASS J21403574+5734550.

We did not detect any periodicity in the variability of 2MASS J21381703+5739265 or 2MASS J21403574+5734550.

3.3.2MASS J21382596+5734093 and 2MASS J21393612+5731289

TheBV(RI)clight curves of 2MASS J21382596+5734093 and 2MASS J21393612+5731289 constructed based on our observations are plotted in Figures 5 and 6 respectively.

It is seen from Figure 5 that from the beginning of our monitoring until 2014 the photometric behavior of 2MASS J21382596+5734093 is characterized by low amplitude variability.After 2014,the star began to exhibit irregular fading events with different amplitudes in all-optical passbands.The star’s color−magnitude diagrams (Figure 5)showed that regardless of the different photometric behaviors before and after 2014,during the whole time of our observations,2MASS J21382596+5734093 became redder as it faded.

Figure 5. BVRcIc light curves (left) and color−magnitude diagrams (right) of 2MASS J21382596+5734093.

Figure 6. BVRcIc light curves of 2MASS J21393612+5731289.

Our time series analysis of the data for this star gave a positive result.We identified a rotational period of 0.9030din its variability.This result confirms the star’s periodicity given in the Zwicky Transient Facility (ZTF) Catalog of Periodic Variable Stars (Chen et al.2020).Figure 7 displays the periodogram and the phasedIcandBlight curves of the star from our observations.In the figure,the circles mark the photometric data of the star until 2014,and the empty triangles represent the photometric data after 2014.

Figure 7.Left: Periodogram of 2MASS J21382596+5734093.Right: Ic and B band phased light curves of the star.The circles in the right panel signify the star’s photometric data until 2014 and the empty triangles mark the ones after 2014.

For 2MASS J21393612+5731289 the available data suggest that it exhibits rapid light variation and its brightness generally varies around some intermediate level in all-optical passbands.The registered photometric amplitudes of the star’s light variations are given in Table 3.Our time-series analysis of the data on the star indicate a rotational period of 1.4919d.The ZTF Catalog of Periodic Variable Stars (Chen et al.2020) gives a period of 2.9838dfor the star’s variability and classifies it as an EW-type eclipsing binary star.As is seen,this is twice the period registered by us and this value corresponds to the second peak in our periodogram.Figure 8 shows the periodogram and the phasedIclight curves of the star according to both identified periods.In the International Variable Star Index database of AAVSO,the periodicity of the star given is half the ZTF catalog value,i.e.,the value corresponding to the first peak in our periodogram.

Figure 8.TOP: Periodogram of 2MASS J21393612+5731289.Bottom:Ic band phased light curves of the star according to both periods.

Figure 10. BVRcIc light curves (left) and color−magnitude diagrams (right) of 2MASS J21393480+5723277.

Figure 11. BVRcIc light curves (left) and color−magnitude diagrams (right) of 2MASS J21403134+5733417.

It is important to mention that the registered periodicity in the photometric behavior of 2MASS J21382596+5734093 and 2MASS J21393612+5731289 remained stable during the whole time of our observations (about 18 yr),and it is a typical rotational period for a WTTS.Most probably the periodicity is caused by rotation modulation of cool spot(s) on the stellar surface.

3.4.2MASS J21383255+5730161,2MASS J21393480+5723277 and 2MASS J21403134+5733417

TheBV(RI)clight curves of 2MASS J21383255+5730161,2MASS J21393480+5723277 and 2MASS J21403134+5733417 from our monitoring are depicted in Figures 9,10 and 11,respectively.As can be seen from the figures,the variability of these stars is characterized by multiple fading events with different amplitudes.For 2MASS J21383255+5730161 these events are distinguishable,but for 2MASS J21393480+5723277 and 2MASS J21403134+5733417 the periods of the dip events are relatively short and sometimes we have only one photometric point in their brightness minima.

The registered amplitudes of the light variations of 2MASS J21383255+5730161,2MASS J21393480+5723277 and 2MASS J21403134+5733417 are given in Table 3.As can be seen,the brightness of the stars varies in wide ranges.The large amplitude dips in brightness are an indication of UXor type variability.In this case,it can be assumed that at least one of the reasons for the photometric variability of 2MASS J21383255+5730161,2MASS J21393480+5723277 and 2MASS J21403134+5733417 is the variable extinction.

During our photometric monitoring,we registered a change in the color of 2MASS J21383255+5730161,2MASS J21393480+5723277 and 2MASS J21403134+5733417 at their brightness minima (Figures 9,10,11).It is seen that initially these stars become redder as they fade,but during the minima in their brightness,the blueing effect is registered.It can be assumed that at least one of the causes for the registered dips in the photometric behavior of the stars is the variation in the density of dust and clouds in orbit around the star,which crossed the line of sight and obscured the objects.We did not detect any periodicity in the variability of 2MASS J21383255+5730161,2MASS J21393480+5723277 or 2MASS J21403134+5733417.

4.Concluding Remarks

We investigated theBV(RI)cphotometric variability of eight young stars in the young open stellar cluster Trumpler 37.All stars from our study manifest typical PMS stars’ photometric variability.The main results of our study are as follows: (i)2MASS J21365072+5731106 (LkHα 349) exhibits photometric variability with amplitude under 0.2 mag in all-optical passbands,typical for WTTSs and HAEBEs.For more than 50 yr,the star’s brightness maintained the same level.(ii)2MASS J21381703+5739265 and 2MASS J21403574+5734550 manifest strong irregular variability,typical for TTSs.(iii) 2MASS J21382596+5734093 and 2MASS J21393612+5731289 show rapid brightness variation,typical for TTSs,probably caused by rotation modulation of cool spot(s) on the stellar surface.We confirmed the periodicity of 0.9030dfor 2MASS J21382596+5734093 and we registered a periodicity of 1.4919dfor 2MASS J21393612+5731289.(iv) The variability of 2MASS J21383255+5730161,2MASS J21393480+5723277 and 2MASS J21403134+5733417 is characterized by multiple brightness dips,typical for UXor type stars.We plan to continue our photometric multicolor monitoring of the investigated stars during the forthcoming years.

Acknowledgments

This research has made use of NASA’s Astrophysics Data System Abstract Service.The authors thank the Director of Skinakas Observatory Prof.I.Papamastorakis and Prof.I.Papadakis for the award of telescope time.We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research.This work was partly supported by the research fund of the University of Shumen,Bulgaria.We thank the anonymous referee for carefully reading the text and for the useful suggestions and comments that helped to improve the paper.

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