Spectroscopy of a Sample of RV Tauri Stars Without IR Excess

Abstract

We observed high-resolution optical spectra of 11 RV Tauri stars without IR excess, with the primary goal of searching for chemical depletion patterns. Using equivalent widths of absorption lines, we calculated the photospheric parameters and chemical element abundances for five stars in the sample: HD 172810, V399 Cyg, AA Ari, V457 Cyg, and V894 Per. Only the abundance pattern of V457 Cyg suggests depletion. In the spectrum of this star, TiO lines are also observed in the emission, in addition to metal emissions. V457 Cyg is likely a binary system that was once surrounded by a circumbinary disc. In the spectrum of V894 Per, we find a set of spectral lines that appear to belong to another star, corroborating that it is an eclipsing variable rather than an RV Tauri star. The high overabundance of sodium may result from mass transfer within the binary system.

1. Introduction

The main characteristic of RV Tauri type stars is the presence of pulsation caused alternating deep and shallow minima in their light curves. Many of these variables possess a peculiar photospheric abundance pattern called depletion, where chemical elements with high dust condensation temperatures are systematically underabundant. This peculiarity is generally thought to arise from the accretion of gas from a dusty disc [1]. This surrounding structure causes IR excess in the spectral energy distribution of RV Tauri-type objects. Indeed, depletion has been observed primarily in stars that exhibit IR excess [2]. The reason why some RV Tauri stars surrounded by a dusty disc exhibit depletion, while others do not, may be related to the presence of a planet within the disc [3]. However, [2] found a few depleted RV Tauri stars without IR excess.

From the perspective of stellar evolution, RV Tauri objects are thought to be in the post-asymptotic giant branch (post-AGB) or post-red giant branch (post-RGB) phase. Variables that possess IR excess are binaries, and the disc is a result of binary interaction that terminated the AGB or RGB stage. The evolutionary status of RV Tauri stars without IR excess is less clear; these may be either single, low-luminosity post-AGB stars or binary post-RGB stars. In the latter case, it is thought that the disc has already dispersed [4]. Little is known about the evolution of discs surrounding post-AGB and post-RGB stars. The longevity of these structures is supported by the fact that they contain large dust grains with high levels of crystallinity (see, e.g., [5]). The evolution of such discs around evolved stars was modelled by [6], who found that the main factor determining the disc’s lifetime is the evolution of the luminous star in the central binary. When the surface of the central star reaches a temperature of around 3 × 10⁴ K, its X-ray flux causes rapid photoevaporation of the disc. However, significant mass loss from the disc in the form of wind has been observed for discs with central stars that have a surface temperature below 1 × 10⁴ K (see, e.g., [7]).

RV Tauri stars whose discs have already dissipated could provide important clues about the evolution of these circumbinary structures. Finding depletion in a star without IR excess indicates that a disc was present at an earlier time. In this study, we present our spectroscopic observations of such RV Tauri variables and the results of their initial analysis.

2. Observations

We observed high-resolution spectra of 11 RV Tauri-type stars without IR excess, with the primary goal of searching for depletion patterns. These stars were selected from the compilation by [2], focusing on the brightest objects that had not yet been studied via high-resolution spectroscopy. The observations were conducted using the high-resolution Fiber-fed Echelle Spectrograph (FIES; [8]) at the Nordic Optical Telescope and the Vilnius University Echelle Spectrograph (VUES; [9]) at the 1.65-m telescope at the Molėtai Astronomical Observatory. The observations are listed in

Table 1. High-resolution spectroscopic observations of RV Tauri stars without IR excess.

Object	V	Date	Spectrograph	R	Exp. Time (min)
V428 Aur	6.87	19 February 2021	VUES	30,000	135
		3 March 2021		30,000	60
		12 October 2022		30,000	120
HD 172810	8.42	11 September 2022	FIES	46,000	11
V399 Cyg	11.28	11 September 2022	FIES	46,000	134
AA Ari	8.69	12 September 2022	FIES	46,000	12
V360 Peg	8.23	12 September 2022	FIES	46,000	8
HD 143352	9.33	27 February 2023	VUES	30,000	120
DZ UMa	11.14	27 February 2023	VUES	30,000	60
		22 April 2023		30,000	180
		23 April 2023		30,000	180
		24 April 2023		30,000	60
		27 April 2023		30,000	60
V1673 Cyg	11.73	17 August 2023	FIES	25,000	97
V457 Cyg	11.99	17 August 2023	FIES	25,000	123
V362 Aql	11.79	17 August 2023	FIES	25,000	103
V894 Per	11.94	17 August 2023	FIES	25,000	118

. Reduction of the observed spectra was conducted by using automatic pipelines of the respective observatories.

Here, we present the initial results of the spectroscopic analysis for five of the observed stars: HD 172810, V399 Cyg, AA Ari, V457 Cyg, and V894 Per. We use the All-Sky Automated Survey for Supernovae (ASAS-SN; [10,11]) light curves (Figure 1) to ascertain their RV Tauri nature and the pulsation phase that corresponds to the time the spectra were observed. The spectrum of V399 Cyg corresponds to the local light maximum just before dimming. However, close to the time of our spectroscopic observations, this star did not exhibit the typical alternating deep and shallow minima. Nevertheless, RV Tauri-like pulsation was observed for some time before MJD ≈ 59,100. The spectrum of V457 Cyg corresponds to the shallow minimum in the light curve. This star also appears to often pulsate in a semiregular manner instead of in an RV Tauri fashion. The spectrum of V894 Per corresponds to the deep minimum in the light curve, where alternating behaviour is clearly seen at all times. The ASAS-SN light curves of HD 172810 and AA Ari appear to be problematic; therefore, we cannot determine the pulsation phase that corresponds to our spectra and confirm the RV Tauri nature. None of the analysed stars show long-term mean magnitude variation in their light curves. We will present the spectroscopic analysis for the remainder of the observed stars in a future paper.

3. Analysis

The reduced spectra are normalised by dividing them by a spline fitted to interactively placed continuum points. Line lists extracted from the Vienna Atomic Line Database (VALD; [12,13]) are used to identify spectral lines. Radial velocities are estimated using a large number of weak and medium-strength absorption lines in each spectrum and by cross-correlating the line profiles with their mirror profiles. The least blended lines are utilised to measure their equivalent widths (EWs), which are used to derive the chemical element abundances. The calculations are performed using the SPECTRUM code [14] and plane-parallel LTE model atmospheres from the ATLAS grid [15]. For V399 Cyg, the iSpec code [16] is used to interpolate the model atmospheres. The source of the atomic data is VALD. Continuum normalisation, along with the measurement of radial velocities and EWs, is performed using the DECH software1.

The photospheric parameters are determined by employing the standard method of excitation and ionisation balance for iron lines. The effective temperature is found by minimising the dependence of iron abundances on the excitation potential of the respective lines. First, the abundances derived from individual Fe I lines (and additionally, Fe II lines in the case of V894 Per) are plotted as a function of the excitation potential. If a trend between the abundances and excitation potentials is observed, the abundances are recalculated by selecting a model atmosphere with a different effective temperature. This process continues until a model atmosphere that results in no trend is found. Subsequently, the surface gravity is determined by selecting a model atmosphere that yields the same iron abundances derived from Fe I and Fe II lines. In the case of AA Ari, we are unable to find suitable Fe II lines; therefore, the surface gravity is highly uncertain. It is approximately estimated by synthesising several regions of the spectrum and attempting to find the best fit with the observations. The microturbulent velocity is derived in a manner similar to that used for the effective temperature, with the difference being that we minimise the trend with the EW instead of the excitation potential.

4. Results and Discussion

The results for the photospheric parameters and radial velocities are presented in

Table 2. Photospheric parameters and heliocentric radial velocities of the analysed stars.

Object	${\mathit{T}}_{\mathit{eff}}$	log g	${\mathit{V}}_{\mathit{mic}}$	${\mathit{V}}_{\mathit{r}}$
	(K)		(km/s)	(km/s)
HD 172810	4250	2.5	2	−4.1
V399 Cyg	4150	0	2.7	−42.6
AA Ari	4750	2 a	2.8	−43.2
V457 Cyg	5750	0.5	5	−53.4
V894 Per	8000 b	1 b	6.8 b	−64.3 c

^a Uncertain due to lack of suitable Fe II lines. ^b Uncertain due to another star affecting the spectrum. ^c Another set of spectral lines at around −137 km/s visible in the spectrum.

, while the derived abundances are presented in

Table 3. Photospheric abundances of the analysed stars.

	HD 172810			V399 Cyg			AA Ari			V457 Cyg			V894 Per
Ion	[X/H]	N	$\mathbf{\sigma }$	[X/H]	N	$\mathbf{\sigma }$	[X/H]	N	$\mathbf{\sigma }$	[X/H]	N	$\mathbf{\sigma }$	[X/H]	N	$\mathbf{\sigma }$
C I										−0.51	5	0.13
O I	0.49	1		−0.63	2	0.04
Na I	0.25	2	0.02				0.89	1		−0.91	1		1.63	3	0.40
Mg I	−0.03	4	0.15	−0.82	1		−0.19	1		−0.48	2	0.03	0.32	4	0.06
Mg II													0.27	1
Al I	0.20	4	0.24
Si I	0.15	7	0.14				0.13	1		−0.27	14	0.14
Si II													0.42	1
S I										−0.23	4	0.10	0.86	1
K I										−1.03	2	0.09
Ca I	−0.35	10	0.20	−1.42	7	0.07				−1.55	4	0.12
Ca II													0.77	1
Sc I	0.23	6	0.12				1.46	2	0.47
Sc II	0.08	2	0.16	−1.81	1		−0.43	1					0.30	4	0.10
Ti I	0.24	70	0.25	−1.36	7	0.10	0.79	10	0.22
Ti II	−0.07	1		−1.18	6	0.12				−1.41	12	0.13	0.39	14	0.15
V I	0.56	42	0.28	−1.63	7	0.13	0.92	8	0.21
V II													0.32	2	0.09
Cr I	0.10	19	0.13	−1.74	6	0.11	0.59	1
Cr II	−0.10	1								−1.62	2	0.05	0.32	15	0.13
Mn I	0.12	2	0.16	−1.84	4	0.35	1.09	2	0.71	−1.30	2	0.17
Fe I	0.01	160	0.24	−1.47	54	0.14	0.07	35	0.24	−0.91	122	0.19	0.40	21	0.19
Fe II	−0.04	2	0.16	−1.52	6	0.13				−1.02	24	0.17	0.26	26	0.16
Co I	0.28	11	0.14	−1.42	5	0.20
Ni I	0.08	6	0.18	−1.16	18	0.24	−0.49	1		−0.81	14	0.07	0.37	1
Ni II										−0.89	1		0.32	1
Cu I				−1.23	2	0.31
Zn I				−1.42	1					−0.74	2	0.00
Sr I	0.39	1
Y I	0.25	2	0.01				0.77	1
Y II	0.28	2	0.13	−1.70	2	0.06	0.49	1					0.37	5	0.18
Zr I	0.52	9	0.28	−1.34	1		0.71	1					0.51	5	0.10
Nb I	0.78	2	0.39
Mo I	0.35	5	0.10
Ba II													0.41	1
La II	0.70	6	0.33				0.45	1
Ce II	0.52	1		−1.72	2	0.15
Pr II	0.53	3	0.34
Nd II	0.39	5	0.14	−1.36	4	0.24	0.70	2	0.28
Sm II				−1.28	5	0.13

Abundances from [17] are used as a reference for solar values.

.

4.1. HD 172810, V399 Cyg, and AA Ari

The derived abundances of HD 172810, V399 Cyg, and AA Ari show no evidence of depletion. Neutron capture elements in HD 172810 appear to have a slight overabundance ([n/H] = 0.4–0.5), while lighter elements have approximately solar abundances. The enhancement of heavy elements is unlikely to result from intrinsic nucleosynthesis due to the star’s low luminosity [18]. All elements in V399 Cyg have approximately the same abundance ([X/H] ≈−1.5), except for oxygen and magnesium. The lines in the spectrum of AA Ari are broad; the average full width at half maximum (FWHM) corresponds to 28 km/s on the velocity scale (FWHM ≈ 10 km/s for HD 172810 and V399 Cyg). This contributes to the large uncertainty in the abundances, which are calculated using more than two lines only for titanium, vanadium, and iron. While iron has approximately solar abundance, titanium and vanadium have [X/H] = 0.8–0.9.

4.2. V457 Cyg

In the spectrum of V457 Cyg, the absorption lines are also broad—FWHM = 23 km/s on average. Numerous weak metal emission lines are visible in the spectrum, identified as low-excitation lines of mostly vanadium and titanium. We also identify TiO molecule lines in emission (Figure 2). The abundance pattern of V457 Cyg indicates depletion, as the abundance ratios [Zn/Ti] and [S/Ti], which are used to quantify the depletion [2], are 0.67 and 1.18, respectively. Therefore, this star is very likely a binary, and its surface chemical composition results from the accretion from a circumbinary disc that has already dissipated. V457 Cyg is the fourth RV Tauri star without IR excess known to be depleted, with the other three being SS Gem, AZ Sgr, and EQ Cas [2]. However, when examining the abundances of all the elements in the photosphere of V457 Cyg (Figure 3), a more complicated picture emerges. The abundances of silicon and magnesium appear too high to be consistent with the depletion scenario. These can be explained by the initial composition of the star being alpha-enhanced by around 0.5 dex. A similar abundance pattern was found in EQ Cas, which was explained as a consequence of the so-called first ionisation potential (FIP) effect, in which stellar winds preferentially pick up ions over atoms [19,20]. This results in elements with low FIP having lower abundances. However, in the case of V457 Cyg, sodium and potassium abundances appear to be inconsistent with the FIP effect (Figure 4).

4.3. V894 Per

The spectral lines of V894 Per are very broad—FWHM ≈ 38 km/s. The derived abundances show [X/H] ≈ 0.4 on average. The abundance of sodium is considerably larger—[Na/H] ≈ 1.6. Some of the strongest identified ion lines are accompanied by a weaker component that is shifted by around 73 km/s to the short-wavelength side (Figure 5), suggesting that the star is a binary. This supports the idea that V894 Per could be an eclipsing variable instead of an RV Tauri star [22,23,24]. Since the spectrum is contaminated by the light from the other component of the binary, our results for the photospheric parameters and abundances should be regarded as uncertain. Nevertheless, the overabundance of sodium is most likely real and may be a consequence of mass transfer within the binary system [25].