The star V473 Lyr is a short-period cepheid (P = 1.49d) with a very strong modulation of the amplitude on a time scale near 1200d. Previously unpublished photometry is presented. This includes good coverage near the maximum amplitude. The available photometry and radial-velocity measurements going back to 1966 are analyzed with PERIOD04 to examine whether the amplitude variability is caused by beating between close frequencies. In particular, we have looked for the existence of a close frequency triplet with equidistant frequency spacing. This is required by the Combination Mode Hypothesis, which explains equidistant frequency triplets by a combination of two frequencies. The frequency triplet determined by us for V473 Lyr misses equidistancy by 0.00005 ± 0.00001 cd−1.
{"title":"Amplitude variability of the cepheid V473 Lyr","authors":"M. Breger","doi":"10.1553/CIA148S52","DOIUrl":"https://doi.org/10.1553/CIA148S52","url":null,"abstract":"The star V473 Lyr is a short-period cepheid (P = 1.49d) with a very strong modulation of the amplitude on a time scale near 1200d. Previously unpublished photometry is presented. This includes good coverage near the maximum amplitude. The available photometry and radial-velocity measurements going back to 1966 are analyzed with PERIOD04 to examine whether the amplitude variability is caused by beating between close frequencies. In particular, we have looked for the existence of a close frequency triplet with equidistant frequency spacing. This is required by the Combination Mode Hypothesis, which explains equidistant frequency triplets by a combination of two frequencies. The frequency triplet determined by us for V473 Lyr misses equidistancy by 0.00005 ± 0.00001 cd−1.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2006-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123616847","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The history of stellar seismology suggests that observation and theory often take turns advancing our understanding. The recent tripling of the sample of pulsating white dwarfs generated by the Sloan Digital Sky Survey represents a giant leap on the observational side. The time is ripe for a comparable advance on the theoretical side. There are basically two ways we can improve our theoretical understanding of pulsating stars: we can improve the fundamental ingredients of the models, or we can explore the existing models in greater computational detail. For pulsating white dwarfs, much progress has recently been made on both fronts: models now exist that connect the interior structure to its complete evolutionary history, while a method of using parallel computers for global exploration of relatively simple models has also been developed. Future advances in theoretical white dwarf asteroseismology will emerge by combining these two approaches, yielding unprecedented insight into the physics of diffusion, nuclear burning, and mixing.
恒星地震学的历史表明，观测和理论常常轮流推进我们的理解。最近，由斯隆数字巡天(Sloan Digital Sky Survey)产生的脉动白矮星样本增加了两倍，这在观测方面是一个巨大的飞跃。在理论方面取得类似进展的时机已经成熟。基本上有两种方法可以提高我们对脉动恒星的理论理解:我们可以改进模型的基本成分，或者我们可以在更大的计算细节上探索现有的模型。对于脉动白矮星，最近在两个方面都取得了很大进展:现在存在将内部结构与其完整进化历史联系起来的模型，同时也开发了一种使用并行计算机对相对简单模型进行全球探索的方法。理论白矮星星震学的未来发展将通过结合这两种方法而出现，从而对扩散、核燃烧和混合的物理学产生前所未有的见解。
{"title":"The Future of Computational Asteroseismology","authors":"T. Metcalfe","doi":"10.1553/cia150s227","DOIUrl":"https://doi.org/10.1553/cia150s227","url":null,"abstract":"The history of stellar seismology suggests that observation and theory often take turns advancing our understanding. The recent tripling of the sample of pulsating white dwarfs generated by the Sloan Digital Sky Survey represents a giant leap on the observational side. The time is ripe for a comparable advance on the theoretical side. There are basically two ways we can improve our theoretical understanding of pulsating stars: we can improve the fundamental ingredients of the models, or we can explore the existing models in greater computational detail. For pulsating white dwarfs, much progress has recently been made on both fronts: models now exist that connect the interior structure to its complete evolutionary history, while a method of using parallel computers for global exploration of relatively simple models has also been developed. Future advances in theoretical white dwarf asteroseismology will emerge by combining these two approaches, yielding unprecedented insight into the physics of diffusion, nuclear burning, and mixing.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2006-11-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123293496","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
C. Cameron, J. Matthews, J. Rowe, R. Kuschnig, D. Guenther, A. Moffat, S. Rucinski, D. Sasselov, G. Walker, W. Weiss
We present 10.27 hrs of photometry of the roAp star HD 134214 obtained by the MOST 1 satellite. The star is shown to be monoperiodic and oscillating at a frequency of 2948.97 ± 0.55 μHz. This is consistent with earlier ground based photometric campaigns (e.g. Kreidl et al. 1994). We do not detect any of the additional frequencies identified in the recent spectroscopic study by Kurtz et al. (2006) down to an amplitude limit of 0.36 mmag (2σ significance limit).
我们介绍了由MOST 1卫星获得的roAp恒星HD 134214的10.27小时光度测量。这颗恒星是单周期的，振荡频率为2948.97±0.55 μHz。这与早期的地面光度测量活动(如Kreidl et al. 1994)是一致的。我们没有检测到Kurtz等人(2006)在最近的光谱研究中发现的任何额外频率，其幅度限制为0.36毫安(2σ显著性限制)。
{"title":"MOST Photometry of the roAp star HD 134214","authors":"C. Cameron, J. Matthews, J. Rowe, R. Kuschnig, D. Guenther, A. Moffat, S. Rucinski, D. Sasselov, G. Walker, W. Weiss","doi":"10.1553/cia148s57","DOIUrl":"https://doi.org/10.1553/cia148s57","url":null,"abstract":"We present 10.27 hrs of photometry of the roAp star HD 134214 obtained by the MOST 1 satellite. The star is shown to be monoperiodic and oscillating at a frequency of 2948.97 ± 0.55 μHz. This is consistent with earlier ground based photometric campaigns (e.g. Kreidl et al. 1994). We do not detect any of the additional frequencies identified in the recent spectroscopic study by Kurtz et al. (2006) down to an amplitude limit of 0.36 mmag (2σ significance limit).","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2006-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115033475","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
There has been tremendous progress in observing oscillations in solar-type stars. In a few short years we have moved from ambiguous detections to firm measurements. We briefly review the recent results, most of which have come from high-precision Doppler measurements. We also review briefly the results on giant and supergiant stars and the prospects for the future.
{"title":"Observations of solar-like oscillations","authors":"T. Bedding, H. Kjeldsen","doi":"10.1553/cia150s106","DOIUrl":"https://doi.org/10.1553/cia150s106","url":null,"abstract":"There has been tremendous progress in observing oscillations in solar-type stars. In a few short years we have moved from ambiguous detections to firm measurements. We briefly review the recent results, most of which have come from high-precision Doppler measurements. We also review briefly the results on giant and supergiant stars and the prospects for the future.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2006-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123670294","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Period04, an extended version of Period98 by Sperl (1998), is a software package designed for sophisticated time string analysis. In this article we present the User Guide for Period04.
{"title":"Period04 User Guide","authors":"P. Lenz, M. Breger","doi":"10.1553/CIA146S53","DOIUrl":"https://doi.org/10.1553/CIA146S53","url":null,"abstract":"Period04, an extended version of Period98 by Sperl (1998), is a software package designed for sophisticated time string analysis. In this article we present the User Guide for Period04.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2005-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128408074","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
P. V. Cauteren, P. Lampens, C. Robertson, A. Strigachev
We report on new time-series CCD observations for three poorly studied open clusters from the STACC list. The collected light curves in the V lter of a large number of stars per eld have been examined in detail in search for shortperiodic variable stars. In particular we looked for new Scuti-type candidates. First results for the open clusters NGC 1664, NGC 6811 and NGC 7209 are presented.
{"title":"Search for intrinsic variable stars in three open clusters: NGC 1664, NGC 6811 and NGC 7209","authors":"P. V. Cauteren, P. Lampens, C. Robertson, A. Strigachev","doi":"10.1553/CIA146S21","DOIUrl":"https://doi.org/10.1553/CIA146S21","url":null,"abstract":"We report on new time-series CCD observations for three poorly studied open clusters from the STACC list. The collected light curves in the V lter of a large number of stars per eld have been examined in detail in search for shortperiodic variable stars. In particular we looked for new Scuti-type candidates. First results for the open clusters NGC 1664, NGC 6811 and NGC 7209 are presented.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2005-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126753152","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
High-resolution spectroscopic observations taken during 5 consecutive nights of the fast rotating δ Scuti star AV Ceti (v sin i = 188km/s) show the presence of non-radial modes with ` ∼ 10 − 16 and very short periods (ν ∼ 40− 70 c/d) Introduction and Observations The rapidly rotating δ Scuti star AV Ceti has been recently the target of a simultaneous photometric and low-resolution spectroscopic international campaign (Dall et al. 2003). Seven low-degree modes were detected in the frequency range 10-31 c/d. We observed this star with the Coudé Echelle Spectrograph attached at the ESO CAT Telescope during 5 consecutive nights (October 24-30, 1994; Remote Control from Garching headquarters) for about 2.5 consecutive hours per night and 55 spectrograms were collected with exposure times of 10 min and a typical S/N ratio at the continuum level of about 230. They had a resolution of 60000 and cover the region 4494-4513 Å. In this region we have two useful lines to study line profile variations: TiII 4501Å and FeII 4508Å. Fig. 1 shows the average continuum normalized spectrum (upper panel) and the pixel-by-pixel standard deviation (lower panel). Added by editor (MB): The Astronomy and Astrophysics publisher used an incorrect name for the star (AV Cetei instead of AV Ceti) in the title and running head of the Dall et al. paper. The authors of the present publication note: Cetus,-i belongs to the second latin declination (as, for example, Cepheus,-i) : nominative and genitive cases are different (Cephei, Ceti). On the other hand, Doradus,-us belongs to the fourth declination and the genitive is the same as the nominative (γ Doradus, not γ Doradi). For a correct use of abbreviations of constellations see http://www.iau.org/Activities/nomenclature/const.html 34 High-degree non-radial modes in the δ Scuti star AV Ceti Figure 1: Average normalized spectrum (top panel); pixel-by-pixel data standard deviation (lower panel). Data analysis and discussion We can see that the line profiles have variations with a std.dev of about 0.002 of the continuum level. A non-linear least-squares fit of a rotationally broadened Gaussian intrinsic profile, taking also into account the limb darkening, on the two average line profiles supplies v sin i = 188± 1 km/s. The line profile variations were analyzed by means of the Fourier Doppler Imaging Technique (Kennelly et al. 1998; Hao 1998). Fig. 2 shows the twodimensional power spectrum obtained considering all the data in a single time series and merging the information of the two spectral lines. We see that there is a clear clump of modes in the region 10 ≤ ` ≤ 16, 35 ≤ ν ≤ 70 c/d. Because of the very severe aliasing, due to the poor temporal coverage, it is not possible to derive a detection of individual modes. A CLEANed version of this power spectrum is shown in Fig. 3 (gain=0.9, 100 iterations). This figure should be considered only as indicative, and the individual modes cannot be taken at face value, since the poor spectra
对快速旋转的δ Scuti星AV Ceti (v sin i = 188km/s)连续5晚进行的高分辨率光谱观测显示，存在' ~ 10−16和非常短的周期(ν ~ 40−70 c/d)的非径向模式。介绍和观测快速旋转的δ Scuti星AV Ceti最近已成为同时进行的光度测定和低分辨率光谱国际运动的目标(Dall et al. 2003)。在10-31 c/d频率范围内检测到7种低度模态。我们连续5个晚上(1994年10月24-30日;在曝光时间为10分钟、典型信噪比为230的连续水平下，采集了55张声谱图。它们的分辨率为60000，覆盖区域4494-4513 Å。在这个区域，我们有两条有用的线来研究线形变化:TiII 4501Å和FeII 4508Å。图1显示了平均连续统归一化光谱(上图)和逐像素标准差(下图)。编辑补充(MB):天文学和天体物理学出版商在Dall等人的论文标题和正文中使用了错误的恒星名称(AV Cetei而不是AV Ceti)。本出版物的作者指出:Cetus，-i属于第二个拉丁赤星(例如，Cepheus，-i):主格和属格的情况是不同的(Cephei, Ceti)。另一方面，Doradus，-us属于第四赤纬，属格与主格相同(γ Doradus，而不是γ Doradi)。有关星座缩写的正确使用，请参见http://www.iau.org/Activities/nomenclature/const.html 34 δ Scuti星AV Ceti的高度非径向模式图1:平均归一化光谱(顶板);逐像素数据标准差(下图)。数据分析和讨论我们可以看到，在连续体水平的0.002左右的标准差范围内，线条轮廓有变化。旋转加宽高斯本征轮廓的非线性最小二乘拟合，也考虑到边缘变暗，在两条平均线轮廓上提供v sin i = 188±1 km/s。利用傅里叶多普勒成像技术(Kennelly et al. 1998;郝1998)。图2为考虑单个时间序列中所有数据并合并两条谱线信息得到的二维功率谱。我们看到在10≤'≤16,35≤ν≤70 c/d区域有一个明显的模态团。由于非常严重的混叠，由于较差的时间覆盖，不可能得出单个模式的检测。该功率谱的清洗版本如图3所示(增益=0.9,100次迭代)。该图应仅被视为指示性的，单个模式不能被视为表面价值，因为较差的光谱窗口使正确的反褶积成为问题。然而，它清楚地表明，我们应该期待一个非常复杂的脉动模式，具有几个高频率的模式。这是由于快速旋转吗?L. Mantegazza和E. Poretti 35图2:二维傅里叶功率谱。图3:清洗后的二维傅立叶功率谱。天蝎座δ星AV Ceti的高度非径向模式的观测是获得恒星脉动光谱更详尽图像的必要条件。我们还注意到，Dall等人(2003)用光度法探测到的低度模式在我们的功率谱中不会产生相关的模式。这并不一定意味着它们不存在，因为我们的技术对高阶模态更敏感(参见Mantegazza 2000)。参考文献Dall, T.H, Handler, G.， Moalusi, M.B, Frandsen, S. 2003, A&A 410, 983郝，J. 1998, ApJ 500, 440 Kennelly,E.J.等。1998，中国生物医学工程学报，495,440
{"title":"High-degree non-radial modes in the δ Scuti star AV Ceti","authors":"L. Mantegazza, E. Poretti","doi":"10.1553/CIA146S33","DOIUrl":"https://doi.org/10.1553/CIA146S33","url":null,"abstract":"High-resolution spectroscopic observations taken during 5 consecutive nights of the fast rotating δ Scuti star AV Ceti (v sin i = 188km/s) show the presence of non-radial modes with ` ∼ 10 − 16 and very short periods (ν ∼ 40− 70 c/d) Introduction and Observations The rapidly rotating δ Scuti star AV Ceti has been recently the target of a simultaneous photometric and low-resolution spectroscopic international campaign (Dall et al. 2003). Seven low-degree modes were detected in the frequency range 10-31 c/d. We observed this star with the Coudé Echelle Spectrograph attached at the ESO CAT Telescope during 5 consecutive nights (October 24-30, 1994; Remote Control from Garching headquarters) for about 2.5 consecutive hours per night and 55 spectrograms were collected with exposure times of 10 min and a typical S/N ratio at the continuum level of about 230. They had a resolution of 60000 and cover the region 4494-4513 Å. In this region we have two useful lines to study line profile variations: TiII 4501Å and FeII 4508Å. Fig. 1 shows the average continuum normalized spectrum (upper panel) and the pixel-by-pixel standard deviation (lower panel). Added by editor (MB): The Astronomy and Astrophysics publisher used an incorrect name for the star (AV Cetei instead of AV Ceti) in the title and running head of the Dall et al. paper. The authors of the present publication note: Cetus,-i belongs to the second latin declination (as, for example, Cepheus,-i) : nominative and genitive cases are different (Cephei, Ceti). On the other hand, Doradus,-us belongs to the fourth declination and the genitive is the same as the nominative (γ Doradus, not γ Doradi). For a correct use of abbreviations of constellations see http://www.iau.org/Activities/nomenclature/const.html 34 High-degree non-radial modes in the δ Scuti star AV Ceti Figure 1: Average normalized spectrum (top panel); pixel-by-pixel data standard deviation (lower panel). Data analysis and discussion We can see that the line profiles have variations with a std.dev of about 0.002 of the continuum level. A non-linear least-squares fit of a rotationally broadened Gaussian intrinsic profile, taking also into account the limb darkening, on the two average line profiles supplies v sin i = 188± 1 km/s. The line profile variations were analyzed by means of the Fourier Doppler Imaging Technique (Kennelly et al. 1998; Hao 1998). Fig. 2 shows the twodimensional power spectrum obtained considering all the data in a single time series and merging the information of the two spectral lines. We see that there is a clear clump of modes in the region 10 ≤ ` ≤ 16, 35 ≤ ν ≤ 70 c/d. Because of the very severe aliasing, due to the poor temporal coverage, it is not possible to derive a detection of individual modes. A CLEANed version of this power spectrum is shown in Fig. 3 (gain=0.9, 100 iterations). This figure should be considered only as indicative, and the individual modes cannot be taken at face value, since the poor spectra","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2005-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124340784","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Note on the short-period variability of V521 Cas in NGC 7789","authors":"P. V. Cauteren, P. Lampens, A. Pigulski","doi":"10.1553/CIA144S23","DOIUrl":"https://doi.org/10.1553/CIA144S23","url":null,"abstract":"Recent observations of V521 Cas in the open cluster NGC7789 do not conflrm that the star is a ‐ Scuti variable (within the observational limits).","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2004-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115677382","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
T. Arentoft, L. Freyhammer, M. Bouzid, C. Sterken, S. Frandsen
We report studies that are carried out with the aim of searching for and studying short-period variable stars in northern open clusters. The background for these studies is described along with the results that have been obtained up to now.
{"title":"Pulsating stars in open clusters","authors":"T. Arentoft, L. Freyhammer, M. Bouzid, C. Sterken, S. Frandsen","doi":"10.1553/CIA145S65","DOIUrl":"https://doi.org/10.1553/CIA145S65","url":null,"abstract":"We report studies that are carried out with the aim of searching for and studying short-period variable stars in northern open clusters. The background for these studies is described along with the results that have been obtained up to now.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2004-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130209164","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
New BVRI CCD observations of the pulsating star SZ Lyn are presented. The light curves are analyzed using Fourier transform techniques and a new period is determined. A new ephemeris, based on recent times of maxima, is proposed. The photometric data collected over the last 40 years are used to determine the pulsational and orbital elements, since SZ Lyncis is a member of a binary system. The results are compared with those found in previous studies.
{"title":"SZ Lyn: New BVRI CCD observations and improved pulsational and orbital elements","authors":"K. Gazeas, P. Niarchos, K. Boutsia","doi":"10.1553/cia144s26","DOIUrl":"https://doi.org/10.1553/cia144s26","url":null,"abstract":"New BVRI CCD observations of the pulsating star SZ Lyn are presented. The light curves are analyzed using Fourier transform techniques and a new period is determined. A new ephemeris, based on recent times of maxima, is proposed. The photometric data collected over the last 40 years are used to determine the pulsational and orbital elements, since SZ Lyncis is a member of a binary system. The results are compared with those found in previous studies.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2004-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116453615","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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